The thermal continuum emission observed from accreting black holes across X-ray bands has the potential to be leveraged as a
powerful probe of the mass and spin of the central black hole. The vast majority of existing ‘continuum fitting’ models neglect
emission sourced at and within the innermost stable circular orbit (ISCO) of the black hole. Numerical simulations, however,
find non-zero emission sourced from these regions. In this work, we extend existing techniques by including the emission
sourced from within the plunging region, utilizing new analytical models that reproduce the properties of numerical accretion
simulations. We show that in general the neglected intra-ISCO emission produces a hot-and-small quasi-blackbody component,
but can also produce a weak power-law tail for more extreme parameter regions. A similar hot-and-small blackbody component
has been added in by hand in an ad hoc manner to previous analyses of X-ray binary spectra. We show that the X-ray spectrum
of MAXI J1820+070 in a soft-state outburst is extremely well described by a full Kerr black hole disc, while conventional
models that neglect intra-ISCO emission are unable to reproduce the data. We believe this represents the first robust detection of
intra-ISCO emission in the literature, and allows additional constraints to be placed on the MAXI J1820 + 070 black hole spin
which must be low a• < 0.5 to allow a detectable intra-ISCO region. Emission from within the ISCO is the dominant emission
component in the MAXI J1820 + 070 spectrum between 6 and 10 keV, highlighting the necessity of including this region. Our
continuum fitting model is made publicly available.
This document summarizes the results of an MHD simulation coupled with a radiation transport model to simulate X-ray spectra from an accreting black hole. Key points:
- For the first time, the simulation is able to reproduce the main components seen in observed X-ray spectra, including a thermal peak, power-law tail, reflection hump, and iron line, by varying only the mass accretion rate.
- The temperature in the corona varies from 10 keV near the disk to over 100 keV in low-density regions, producing the hard X-ray emission through inverse-Compton scattering.
- Even as the disk's reflection edge varies from the horizon out to 6 gravitational radii with decreasing accretion
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
Todo mundo sabe que os raios produzidos pela Estrela da Morte em Guerra nas Estrelas não pode existir na vida real, porém no universo existem fenômenos que as vezes conseguem superar até a mais surpreendente ficção.
A galáxia Pictor A, é um desses objetos que possuem fenômenos tão espetaculares quanto aqueles exibidos no cinema. Essa galáxia localiza-se a cerca de 500 milhões de anos-luz da Terra e possui um buraco negro supermassivo no seu centro. Uma grande quantidade de energia gravitacional é lançada, à medida que o material cai em direção ao horizonte de eventos, o ponto sem volta ao redor do buraco negro. Essa energia produz um enorme jato de partículas que viajam a uma velocidade próxima da velocidade da luz no espaço intergaláctico, chamado de jato relativístico.
Para obter imagens desse jato, os cientistas usaram o Observatório de Raios-X Chandra, da NASA várias vezes durante 15 anos. Os dados do Chandra, apresentados em azul nas imagens, foram combinados com os dados obtidos em ondas de rádio a partir do Australia Telescope Compact Array, e são aparesentados em vermelho nas imagens.
X-rays from a Central “Exhaust Vent” of the Galactic Center ChimneySérgio Sacani
Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of
linear X-ray-emitting features located within the southern portion of the Galactic center chimney,
and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08◦
, b = −1.42◦
. The
surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may
have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the
feature’s spectra favor a complex two-component model consisting of thermal and recombining plasma
components, possibly a sign of shock compression or heating of the interstellar medium by outflowing
material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this
plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a
sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy
source to sustain the observed morphology
Spirals and clumps in V960 Mon: signs of planet formation via gravitational i...Sérgio Sacani
The formation of giant planets has traditionally been divided into two pathways: core accretion and gravitational instability. However, in recent years, gravitational instability has become less favored, primarily due
to the scarcity of observations of fragmented protoplanetary disks around young stars and low occurrence rate
of massive planets on very wide orbits. In this study, we present a SPHERE/IRDIS polarized light observation
of the young outbursting object V960 Mon. The image reveals a vast structure of intricately shaped scattered
light with several spiral arms. This finding motivated a re-analysis of archival ALMA 1.3 mm data acquired
just two years after the onset of the outburst of V960 Mon. In these data, we discover several clumps of continuum emission aligned along a spiral arm that coincides with the scattered light structure. We interpret the
localized emission as fragments formed from a spiral arm under gravitational collapse. Estimating the mass of
solids within these clumps to be of several Earth masses, we suggest this observation to be the first evidence of
gravitational instability occurring on planetary scales. This study discusses the significance of this finding for
planet formation and its potential connection with the outbursting state of V960 Mon.
Detection of anisotropic satellite quenching in galaxy clusters up to z ∼ 1Sérgio Sacani
Satellite galaxies in the cluster environment are more likely to be quenched than galaxies in the general field. Recently, it has
been reported that satellite galaxy quenching depends on the orientation relative to their central galaxies: satellites along the
major axis of centrals are more likely to be quenched than those along the minor axis. In this paper, we report a detection
of such anisotropic quenching up to z ∼ 1 based on a large optically selected cluster catalogue constructed from the Hyper
Suprime-Cam Subaru Strategic Program. We calculate the quiescent satellite galaxy fraction as a function of orientation angle
measured from the major axis of central galaxies and find that the quiescent fractions at 0.25 < z < 1 are reasonably fitted
by sinusoidal functions with amplitudes of a few per cent. Anisotropy is clearer in inner regions (<r200m) of clusters and not
significant in cluster outskirts (>r200m). We also confirm that the observed anisotropy cannot be explained by differences in
local galaxy density or stellar mass distribution along the two axes. Quiescent fraction excesses between the two axes suggest
that the quenching efficiency contributing to the anisotropy is almost independent of stellar mass, at least down to our stellar
mass limit of M∗ = 1 × 1010 M. Finally, we argue that the physical origins of the observed anisotropy should have shorter
quenching time-scales than ∼ 1 Gyr, like ram-pressure stripping, because, for anisotropic quenching to be observed, satellites
must be quenched before their initial orientation angles are significantly changed.
Measuring the Hubble constant with kilonovae using the expanding photosphere ...Sérgio Sacani
While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of
the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding
atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement
to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the
major uncertainties commonly associated with this method in supernovae: (1) the early continuum is very well-reproduced by a
blackbody spectrum, (2) the dilution effect from electron scattering opacity is likely negligible, (3) the explosion times are exactly
known due to the GW detection, and (4) the ejecta geometry is, at least in some cases, highly spherical and can be constrained from
line-shape analysis. We provide an analysis of the early VLT/X-shooter spectra AT2017gfo showing how the luminosity distance can
be determined, and find a luminosity distance of DL = 44.5 ± 0.8 Mpc in agreement with, but more precise than, previous methods.
We investigate the dominant systematic uncertainties, but our simple framework, which assumes a blackbody photosphere, does not
account for the full time-dependent three-dimensional radiative transfer effects, so this distance should be treated as preliminary. The
luminosity distance corresponds to an estimated Hubble constant of H0 = 67.0 ± 3.6 km s−1 Mpc−1
, where the dominant uncertainty
is due to the modelling of the host peculiar velocity. We also estimate the expected constraints on H0 from future KN-EPM-analysis
with the upcoming O4 and O5 runs of the LIGO collaboration GW-detectors, where five to ten similar KNe would yield 1% precision
cosmological constraints.
This document summarizes the results of an MHD simulation coupled with a radiation transport model to simulate X-ray spectra from an accreting black hole. Key points:
- For the first time, the simulation is able to reproduce the main components seen in observed X-ray spectra, including a thermal peak, power-law tail, reflection hump, and iron line, by varying only the mass accretion rate.
- The temperature in the corona varies from 10 keV near the disk to over 100 keV in low-density regions, producing the hard X-ray emission through inverse-Compton scattering.
- Even as the disk's reflection edge varies from the horizon out to 6 gravitational radii with decreasing accretion
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
Todo mundo sabe que os raios produzidos pela Estrela da Morte em Guerra nas Estrelas não pode existir na vida real, porém no universo existem fenômenos que as vezes conseguem superar até a mais surpreendente ficção.
A galáxia Pictor A, é um desses objetos que possuem fenômenos tão espetaculares quanto aqueles exibidos no cinema. Essa galáxia localiza-se a cerca de 500 milhões de anos-luz da Terra e possui um buraco negro supermassivo no seu centro. Uma grande quantidade de energia gravitacional é lançada, à medida que o material cai em direção ao horizonte de eventos, o ponto sem volta ao redor do buraco negro. Essa energia produz um enorme jato de partículas que viajam a uma velocidade próxima da velocidade da luz no espaço intergaláctico, chamado de jato relativístico.
Para obter imagens desse jato, os cientistas usaram o Observatório de Raios-X Chandra, da NASA várias vezes durante 15 anos. Os dados do Chandra, apresentados em azul nas imagens, foram combinados com os dados obtidos em ondas de rádio a partir do Australia Telescope Compact Array, e são aparesentados em vermelho nas imagens.
X-rays from a Central “Exhaust Vent” of the Galactic Center ChimneySérgio Sacani
Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of
linear X-ray-emitting features located within the southern portion of the Galactic center chimney,
and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08◦
, b = −1.42◦
. The
surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may
have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the
feature’s spectra favor a complex two-component model consisting of thermal and recombining plasma
components, possibly a sign of shock compression or heating of the interstellar medium by outflowing
material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this
plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a
sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy
source to sustain the observed morphology
Spirals and clumps in V960 Mon: signs of planet formation via gravitational i...Sérgio Sacani
The formation of giant planets has traditionally been divided into two pathways: core accretion and gravitational instability. However, in recent years, gravitational instability has become less favored, primarily due
to the scarcity of observations of fragmented protoplanetary disks around young stars and low occurrence rate
of massive planets on very wide orbits. In this study, we present a SPHERE/IRDIS polarized light observation
of the young outbursting object V960 Mon. The image reveals a vast structure of intricately shaped scattered
light with several spiral arms. This finding motivated a re-analysis of archival ALMA 1.3 mm data acquired
just two years after the onset of the outburst of V960 Mon. In these data, we discover several clumps of continuum emission aligned along a spiral arm that coincides with the scattered light structure. We interpret the
localized emission as fragments formed from a spiral arm under gravitational collapse. Estimating the mass of
solids within these clumps to be of several Earth masses, we suggest this observation to be the first evidence of
gravitational instability occurring on planetary scales. This study discusses the significance of this finding for
planet formation and its potential connection with the outbursting state of V960 Mon.
Detection of anisotropic satellite quenching in galaxy clusters up to z ∼ 1Sérgio Sacani
Satellite galaxies in the cluster environment are more likely to be quenched than galaxies in the general field. Recently, it has
been reported that satellite galaxy quenching depends on the orientation relative to their central galaxies: satellites along the
major axis of centrals are more likely to be quenched than those along the minor axis. In this paper, we report a detection
of such anisotropic quenching up to z ∼ 1 based on a large optically selected cluster catalogue constructed from the Hyper
Suprime-Cam Subaru Strategic Program. We calculate the quiescent satellite galaxy fraction as a function of orientation angle
measured from the major axis of central galaxies and find that the quiescent fractions at 0.25 < z < 1 are reasonably fitted
by sinusoidal functions with amplitudes of a few per cent. Anisotropy is clearer in inner regions (<r200m) of clusters and not
significant in cluster outskirts (>r200m). We also confirm that the observed anisotropy cannot be explained by differences in
local galaxy density or stellar mass distribution along the two axes. Quiescent fraction excesses between the two axes suggest
that the quenching efficiency contributing to the anisotropy is almost independent of stellar mass, at least down to our stellar
mass limit of M∗ = 1 × 1010 M. Finally, we argue that the physical origins of the observed anisotropy should have shorter
quenching time-scales than ∼ 1 Gyr, like ram-pressure stripping, because, for anisotropic quenching to be observed, satellites
must be quenched before their initial orientation angles are significantly changed.
Measuring the Hubble constant with kilonovae using the expanding photosphere ...Sérgio Sacani
While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of
the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding
atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement
to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the
major uncertainties commonly associated with this method in supernovae: (1) the early continuum is very well-reproduced by a
blackbody spectrum, (2) the dilution effect from electron scattering opacity is likely negligible, (3) the explosion times are exactly
known due to the GW detection, and (4) the ejecta geometry is, at least in some cases, highly spherical and can be constrained from
line-shape analysis. We provide an analysis of the early VLT/X-shooter spectra AT2017gfo showing how the luminosity distance can
be determined, and find a luminosity distance of DL = 44.5 ± 0.8 Mpc in agreement with, but more precise than, previous methods.
We investigate the dominant systematic uncertainties, but our simple framework, which assumes a blackbody photosphere, does not
account for the full time-dependent three-dimensional radiative transfer effects, so this distance should be treated as preliminary. The
luminosity distance corresponds to an estimated Hubble constant of H0 = 67.0 ± 3.6 km s−1 Mpc−1
, where the dominant uncertainty
is due to the modelling of the host peculiar velocity. We also estimate the expected constraints on H0 from future KN-EPM-analysis
with the upcoming O4 and O5 runs of the LIGO collaboration GW-detectors, where five to ten similar KNe would yield 1% precision
cosmological constraints.
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068Sérgio Sacani
Multiwavelength observations indicate that some starburst galaxies show a dominant nonthermal contribution from
their central region. These active galactic nuclei (AGN)-starburst composites are of special interest, as both
phenomena on their own are potential sources of highly energetic cosmic rays and associated γ-ray and neutrino
emission. In this work, a homogeneous, steady-state two-zone multimessenger model of the nonthermal emission
from the AGN corona as well as the circumnuclear starburst region is developed and subsequently applied to the
case of NGC 1068, which has recently shown some first indications of high-energy neutrino emission. Here, we
show that the entire spectrum of multimessenger data—from radio to γ-rays including the neutrino constraint—can
be described very well if both, starburst and AGN corona, are taken into account. Using only a single emission
region is not sufficient.
This document summarizes the results of a 180 ks Chandra-LETGS observation of Mrk 509 as part of a larger multi-wavelength campaign. The observation detected several absorption features in the X-ray spectrum originating from an ionized absorber, including ions with three distinct ionization degrees. The lowest ionized component is slightly redshifted and not in pressure equilibrium with the others, likely belonging to the host galaxy's interstellar medium. The other two components are outflowing at velocities of around -200 and -455 km/s. Simultaneous HST-COS observations detected 13 UV kinematic components, and at least three can be associated with the X-ray components, providing evidence that the UV and X-
Dust in the_polar_region_as_a_major_contributor_to_the_infrared_emission_of_a...Sérgio Sacani
The mid-infrared emission of the active galactic nucleus NGC 3783 was observed using interferometry over multiple epochs, providing dense coverage of position angles and baselines. The emission was found to be strongly elongated along a position angle of -52 degrees, closely aligned with the polar axis orientation of -45 degrees. The half-light radii were measured to be 20.0 mas by 6.7 mas, corresponding to an axis ratio of 3:1. This implies that 60-90% of the 8-13 micron emission is from the polar-elongated component. The observations support a scenario where the majority of mid-infrared emission in Seyfert galaxies originates from a dusty wind in the polar region,
This document numerically analyzes the wave function of atoms under the combined effects of an optical lattice trapping potential and a harmonic oscillator potential, as used in Bose-Einstein condensation experiments. It employs the Crank-Nicolson scheme to solve the Gross-Pitaevskii equation. The results show that the wave function distribution responds to parameters like the trapping frequencies ratio, optical lattice intensity, chemical potential, and energy. Careful adjustment of the time step and grid spacing is needed to satisfy conservation of norms and energy as required by the physical system. Distributions of the overlapping potentials for different q-factors are presented.
The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in...Sérgio Sacani
SMSS J114447.77-430859.3 (z = 0.83) has been identified in the SkyMapper Southern Survey as the most luminous quasar in
the last ∼ 9 Gyr . In this paper, we report on the eROSITA/Spectrum–Roentgen–Gamma (SRG) observations of the source from
the eROSITA All Sky Survey, along with presenting results from recent monitoring performed using Swift, XMM-Newton, and
NuSTAR. The source shows a clear variability by factors of ∼10 and ∼2.7 overtime-scales of a year and of a few days,respectively.
When fit with an absorbed power law plus high-energy cutoff, the X-ray spectra reveal a = 2.2 ± 0.2 and Ecut = 23+26
−5 keV
. Assuming Comptonization, we estimate a coronal optical depth and electron temperature of τ = 2.5 − 5.3 (5.2 − 8) and
kT = 8 − 18 (7.5 − 14) keV , respectively, for a slab (spherical) geometry. The broadband SED is successfully modelled by
assuming either a standard accretion disc illuminated by a central X-ray source, or a thin disc with a slim disc emissivity profile.
The former model results in a black hole mass estimate of the order of 1010 M , slightly higher than prior optical estimates;
meanwhile, the latter model suggests a lower mass. Both models suggest sub-Eddington accretion when assuming a spinning
black hole, and a compact (∼ 10 rg ) X-ray corona. The measured intrinsic column density and the Eddington ratio strongly
suggest the presence of an outflow driven by radiation pressure. This is also supported by variation of absorption by an order of
magnitude over the period of ∼ 900 d .
Serendipitous discovery of an extended xray jet without a radio counterpart i...Sérgio Sacani
A recent Chandra observation of the nearby galaxy cluster Abell 585 has led to the discovery of
an extended X-ray jet associated with the high-redshift background quasar B3 0727+409, a luminous
radio source at redshift z = 2:5. This is one of only few examples of high-redshift X-ray jets known
to date. It has a clear extension of about 1200, corresponding to a projected length of 100 kpc, with
a possible hot spot located 3500 from the quasar. The archival high resolution VLA maps surprisingly
reveal no extended jet emission, except for one knot about 1:400 from the quasar. The high X-ray to
radio luminosity ratio for this source appears consistent with the / (1 + z)4 amplication expected
from the inverse Compton radiative model. This serendipitous discovery may signal the existence
of an entire population of similar systems with bright X-ray and faint radio jets at high redshift, a
selection bias which must be accounted for when drawing any conclusions about the redshift evolution
of jet properties and indeed about the cosmological evolution of supermassive black holes and active
galactic nuclei in general.
Radio continum emission_of_35_edge_on_galaxies_observed_with_the_vlaSérgio Sacani
Usando um dos maiores rádio observatórios do mundo, o Very Large Array do National Radio Astronomy, um grupo de astrônomos descobriram que os halos ao redor dos discos das galáxias espirais são muito mais comuns do que se pensava anteriormente.
A equipe, dirigida pela Dra. Judith Irwin, da Universidade de Queens, em Kingston, ON, Canadá, observou 35 galáxias espirais próximas de lado, de 11 a 137 milhões de anos-luz de distância da Terra.
As galáxias espirais, como a nossa própria Via Láctea ou a famosa Galáxia de Andrômeda, possuem uma vasta maioria de suas estrelas, gás, e poeira num disco plano em rotação com braços espirais. A maior parte da luz e das ondas de rádio observadas com telescópios veem de objetos localizados nesse disco.
“Nós sabíamos antes que alguns halos existiam, mas, usando o poder total do VLA atualizado e o poder total de algumas técnicas de processamento de imagens, nós descobrimos que esses halos são muito mais comuns entre as galáxias espirais do que nós pensávamos antes”, explicou a Dra. Irwin.
3D-Spatiotemporal forecasting the expansion of supernova shells using deep le...Sérgio Sacani
Supernova (SN) plays an important role in galaxy formation and evolution. In high-resolution galaxy simulations using massively
parallel computing, short integration time-steps for SNe are serious bottlenecks. This is an urgent issue that needs to be resolved
for future higher-resolution galaxy simulations. One possible solution would be to use the Hamiltonian splitting method, in
which regions requiring short time-steps are integrated separately from the entire system. To apply this method to the particles
affected by SNe in a smoothed particle hydrodynamics simulation, we need to detect the shape of the shell on and within which
such SN-affected particles reside during the subsequent global step in advance. In this paper, we develop a deep learning model,
3D-Memory In Memory (3D-MIM), to predict a shell expansion after a SN explosion. Trained on turbulent cloud simulations
with particle mass mgas = 1 M, the model accurately reproduces the anisotropic shell shape, where densities decrease by over
10 per cent by the explosion. We also demonstrate that the model properly predicts the shell radius in the uniform medium
beyond the training data set of inhomogeneous turbulent clouds. We conclude that our model enables the forecast of the shell
and its interior where SN-affected particles will be present.
A Comprehensive Theory for Neutron Star and Black Hole Kicks and Induced SpinsSérgio Sacani
Using twenty long-term 3D core-collapse supernova simulations, we find that lower compactness progenitors that explode quasi-spherically due to the short delay to explosion experience smaller neutron
star recoil kicks in the ∼100−200 km s−1
range, while higher compactness progenitors that explode
later and more aspherically leave neutron stars with kicks in the ∼300−1000 km s−1
range. In addition, we find that these two classes are correlated with the gravitational mass of the neutron star.
This correlation suggests that the survival of binary neutron star systems may in part be due to their
lower kick speeds. We also find a correlation of the kick with both the mass dipole of the ejecta
and the explosion energy. Furthermore, one channel of black hole birth leaves masses of ∼10 M⊙, is
not accompanied by a neutrino-driven explosion, and experiences small kicks. A second is through
a vigorous explosion that leaves behind a black hole with a mass of ∼3.0 M⊙ kicked to high speeds.
We find that the induced spins of nascent neutron stars range from seconds to ∼10 milliseconds and
that a spin/kick correlation for pulsars emerges naturally. We suggest that if an initial spin biases
the explosion direction, a spin/kick correlation is a common byproduct of the neutrino mechanism of
core-collapse supernovae. Finally, the induced spin in explosive black hole formation is likely large and
in the collapsar range. This new 3D model suite provides a greatly expanded perspective and appears
to explain some observed pulsar properties by default.
First identification of_direct_collapse_black_holes_candidates_in_the_early_u...Sérgio Sacani
The first black hole seeds, formed when the Universe was younger than ⇠ 500Myr, are recognized
to play an important role for the growth of early (z ⇠ 7) super-massive black holes.
While progresses have been made in understanding their formation and growth, their observational
signatures remain largely unexplored. As a result, no detection of such sources has been
confirmed so far. Supported by numerical simulations, we present a novel photometric method
to identify black hole seed candidates in deep multi-wavelength surveys.We predict that these
highly-obscured sources are characterized by a steep spectrum in the infrared (1.6−4.5μm),
i.e. by very red colors. The method selects the only 2 objects with a robust X-ray detection
found in the CANDELS/GOODS-S survey with a photometric redshift z & 6. Fitting their
infrared spectra only with a stellar component would require unrealistic star formation rates
(& 2000M# yr−1). To date, the selected objects represent the most promising black hole seed
candidates, possibly formed via the direct collapse black hole scenario, with predicted mass
> 105M#. While this result is based on the best photometric observations of high-z sources
available to date, additional progress is expected from spectroscopic and deeper X-ray data.
Upcoming observatories, like the JWST, will greatly expand the scope of this work.
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...Sérgio Sacani
The document discusses asymmetrical tidal tails observed around five open star clusters, which challenges Newtonian gravity. It summarizes how tidal tails form as stars escape clusters due to energy equipartition. Observations of the Hyades, Praesepe, Coma Berenices, COIN-Gaia 13, and NGC 752 clusters found more stars in the leading tidal tails within 50 pc of the clusters. Simulations show that in Newtonian gravity, tidal tails should be symmetrical, but asymmetries can arise in Milgromian dynamics. Future work is needed to better map tidal tails and develop Milgromian simulations.
Formation of low mass protostars and their circumstellar disksSérgio Sacani
Understanding circumstellar disks is of prime importance in astrophysics, however, their birth process remains poorly constrained due to observational and numerical challenges. Recent numerical works have shown that the small-scale physics, often wrapped into a sub-grid model, play a crucial role in disk formation and evolution. This calls for a combined approach in which both the protostar and circumstellar disk are studied in concert. Aims. We aim to elucidate the small scale physics and constrain sub-grid parameters commonly chosen in the literature by resolving the star-disk interaction. Methods. We carry out a set of very high resolution 3D radiative-hydrodynamics simulations that self-consistently describe the collapse of a turbulent dense molecular cloud core to stellar densities. We study the birth of the protostar, the circumstellar disk, and its early evolution (< 6 yr after protostellar formation). Results. Following the second gravitational collapse, the nascent protostar quickly reaches breakup velocity and sheds its surface material, thus forming a hot (∼ 103 K), dense, and highly flared circumstellar disk. The protostar is embedded within the disk, such that material can flow without crossing any shock fronts. The circumstellar disk mass quickly exceeds that of the protostar, and its kinematics are dominated by self-gravity. Accretion onto the disk is highly anisotropic, and accretion onto the protostar mainly occurs through material that slides on the disk surface. The polar mass flux is negligible in comparison. The radiative behavior also displays a strong anisotropy, as the polar accretion shock is shown to be supercritical whereas its equatorial counterpart is subcritical. We also f ind a remarkable convergence of our results with respect to initial conditions. Conclusions. These results reveal the structure and kinematics in the smallest spatial scales relevant to protostellar and circumstellar disk evolution. They can be used to describe accretion onto regions commonly described by sub-grid models in simulations studying larger scale physics.
Hydrogen Column Density Variability in a Sample of Local Compton-Thin AGNSérgio Sacani
We present the analysis of multiepoch observations of a set of 12 variable, Compton-thin, local (z<0.1) active galactic nuclei (AGN) selected from the 100-month BAT catalog. We analyze all available X-ray data from Chandra, XMMNewton, and NuSTAR, adding up to a total of 53 individual observations. This corresponds to between 3 and 7 observations per source, probing variability timescales between a few days and ∼ 20 yr. All sources have at least one NuSTAR observation, ensuring high-energy coverage, which allows us to disentangle the line-of-sight and reflection components in the X-ray spectra. For each source, we model all available spectra simultaneously, using the physical torus models MYTorus, borus02, and UXCLUMPY. The simultaneous fitting, along with the high-energy coverage, allows us to place tight constraints on torus parameters such as the torus covering factor, inclination angle, and torus average column density. We also estimate the line-of-sight column density (NH) for each individual observation. Within the 12 sources, we detect clear line-of-sight NH variability in 5, non-variability in 5, and for 2 of them it is not possible to fully disentangle intrinsic-luminosity and NH variability. We observe large differences between the average values of line-ofsight NH (or NH of the obscurer) and the average NH of the torus (or NH of the reflector), for each source, by a factor between ∼ 2 to > 100. This behavior, which suggests a physical disconnect between the absorber and the reflector, is more extreme in sources that present NH variability. NH-variable AGN also tend to present larger obscuration and broader cloud distributions than their non-variable counterparts. We observe that large changes in obscuration only occur at long timescales, and use this to place tentative lower limits on torus cloud sizes.
This paper analyzes NuSTAR X-ray observations of 9 optically selected type 2 quasars (QSO2s) at z < 0.5 that were candidates for being Compton-thick based on previous observations. Five new NuSTAR observations are reported. Five of the nine QSO2s were detected by NuSTAR in the 8-24 keV band, with three having sufficient counts for spectral modeling. For these three sources, NuSTAR data found their column densities were 2.5-1600 times higher and intrinsic luminosities were 10-70 times higher than previous estimates from Chandra and XMM-Newton alone. Accounting for these corrections, the authors estimate the Compton-thick fraction of optically selected type
Triple Spiral Arms of a Triple Protostar System Imaged in Molecular LinesSérgio Sacani
Most stars form in multiple-star systems. For a better understanding of their formation processes, it is important to
resolve the individual protostellar components and the surrounding envelope and disk material at the earliest
possible formation epoch, because the formation history can be lost in a few orbital timescales. Here we present
Atacama Large Millimeter/submillimeter Array observational results of a young multiple protostellar system,
IRAS 04239+2436, where three well-developed large spiral arms were detected in the shocked SO emission.
Along the most conspicuous arm, the accretion streamer was also detected in the SO2 emission. The observational
results are complemented by numerical magnetohydrodynamic simulations, where those large arms only appear in
magnetically weakened clouds. Numerical simulations also suggest that the large triple spiral arms are the result of
gravitational interactions between compact triple protostars and the turbulent infalling envelope.
M82 X-2 is the first pulsating ultraluminous X-ray source discovered. The luminosity of these extreme pulsars, if
isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but
with an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass
transfer rate can help discriminate between these two scenarios. In this paper, we follow the orbit of the neutron star
for 7 yr, measure the decay of the orbit (P P orb orb 8 10 yr 6 1 · » - - - ), and argue that this orbital decay is driven by
extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. If this is true,
the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also
strongly favors models where the accretor is a highly magnetized neutron star.
ALMA Observations of the Extraordinary Carina Pillars: A Complementary SampleSérgio Sacani
We present a study of six dusty and gaseous pillars (containing the HH 1004 and HH 1010 objects)
and globules (that contain the HH 666, HH 900, HH 1006, and HH 1066 objects) localized in the Carina
nebula using sensitive and high angular resolution (∼0.3′′) Atacama Large Millimeter/Sub-millimeter
Array (ALMA) observations. This is a more extensive study that the one presented in Cortes-Rangel
et al. (2020). As in this former study, we also analyzed the 1.3 mm continuum emission and C18O(2−1),
N2D+(3−2) and 12CO(2−1) spectral lines. These new observations revealed the molecular outflows
emanating from the pillars, the dusty envelopes+disks that are exciting them, and the extended HH
objects far from their respective pillars. We reveal that the masses of the disks+envelopes are in a
range of 0.02 to 0.38 M⊙, and those for the molecular outflows are of the order of 10−3 M⊙, which
suggests that their exciting sources might be low- or intermediate-mass protostars as already revealed
in recent studies at infrared and submillimeter bands. In the regions associated with the objects HH
900 and HH 1004, we report multiple millimeter continuum sources, from where several molecular
outflows emanate.
This document discusses the recycling of magnetic flux in the quiet Sun's corona. It presents a study that uses magnetogram observations to track photospheric magnetic flux fragments over time and models their evolution using a potential field approximation. The main findings are:
1) The quiet Sun's coronal flux is generally recycled on much shorter timescales, around 3 hours, than the corresponding recycling timescale of photospheric flux, which is around 8-19 hours.
2) When also considering emergence and cancellation of photospheric flux, the net replacement time of coronal flux is estimated to be only 1.4 hours.
3) The amount of magnetic reconnection driven by the motions and interactions of photospheric
A propable milli_parsec_supermassive_binary_black_hole_in_the_nearest_quasar_...Sérgio Sacani
Astrônomos usando o Telescópio Espacial Hubble da NASA descobriram que a Markarian 231 (Mrk 231), a galáxia mais próxima da Terra que abriga um quasar, é alimentada por dois buracos negros centrais girando violentamente um em relação ao outro.
A descoberta sugere que os quasares, os brilhantes núcleos das galáxias ativas, podem normalmente abrigar dois buracos negros centrais que caem, um na órbita do outro como resultado da fusão de duas galáxias. Como um par de patinadores, o buraco negro duplo gera uma tremenda quantidade de energia que faz o núcleo da galáxia que o abriga se sobrepor ao brilho da população de bilhões de estrelas da galáxia, que os cientistas então identificam como quasares.
Os cientistas procuraram nas observações de arquivo do Hubble feitas na radiação ultravioleta emitida do centro da Mrk 231 para descobrir o que eles descrevem como propriedades extremas e surpreendentes.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
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Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068Sérgio Sacani
Multiwavelength observations indicate that some starburst galaxies show a dominant nonthermal contribution from
their central region. These active galactic nuclei (AGN)-starburst composites are of special interest, as both
phenomena on their own are potential sources of highly energetic cosmic rays and associated γ-ray and neutrino
emission. In this work, a homogeneous, steady-state two-zone multimessenger model of the nonthermal emission
from the AGN corona as well as the circumnuclear starburst region is developed and subsequently applied to the
case of NGC 1068, which has recently shown some first indications of high-energy neutrino emission. Here, we
show that the entire spectrum of multimessenger data—from radio to γ-rays including the neutrino constraint—can
be described very well if both, starburst and AGN corona, are taken into account. Using only a single emission
region is not sufficient.
This document summarizes the results of a 180 ks Chandra-LETGS observation of Mrk 509 as part of a larger multi-wavelength campaign. The observation detected several absorption features in the X-ray spectrum originating from an ionized absorber, including ions with three distinct ionization degrees. The lowest ionized component is slightly redshifted and not in pressure equilibrium with the others, likely belonging to the host galaxy's interstellar medium. The other two components are outflowing at velocities of around -200 and -455 km/s. Simultaneous HST-COS observations detected 13 UV kinematic components, and at least three can be associated with the X-ray components, providing evidence that the UV and X-
Dust in the_polar_region_as_a_major_contributor_to_the_infrared_emission_of_a...Sérgio Sacani
The mid-infrared emission of the active galactic nucleus NGC 3783 was observed using interferometry over multiple epochs, providing dense coverage of position angles and baselines. The emission was found to be strongly elongated along a position angle of -52 degrees, closely aligned with the polar axis orientation of -45 degrees. The half-light radii were measured to be 20.0 mas by 6.7 mas, corresponding to an axis ratio of 3:1. This implies that 60-90% of the 8-13 micron emission is from the polar-elongated component. The observations support a scenario where the majority of mid-infrared emission in Seyfert galaxies originates from a dusty wind in the polar region,
This document numerically analyzes the wave function of atoms under the combined effects of an optical lattice trapping potential and a harmonic oscillator potential, as used in Bose-Einstein condensation experiments. It employs the Crank-Nicolson scheme to solve the Gross-Pitaevskii equation. The results show that the wave function distribution responds to parameters like the trapping frequencies ratio, optical lattice intensity, chemical potential, and energy. Careful adjustment of the time step and grid spacing is needed to satisfy conservation of norms and energy as required by the physical system. Distributions of the overlapping potentials for different q-factors are presented.
The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in...Sérgio Sacani
SMSS J114447.77-430859.3 (z = 0.83) has been identified in the SkyMapper Southern Survey as the most luminous quasar in
the last ∼ 9 Gyr . In this paper, we report on the eROSITA/Spectrum–Roentgen–Gamma (SRG) observations of the source from
the eROSITA All Sky Survey, along with presenting results from recent monitoring performed using Swift, XMM-Newton, and
NuSTAR. The source shows a clear variability by factors of ∼10 and ∼2.7 overtime-scales of a year and of a few days,respectively.
When fit with an absorbed power law plus high-energy cutoff, the X-ray spectra reveal a = 2.2 ± 0.2 and Ecut = 23+26
−5 keV
. Assuming Comptonization, we estimate a coronal optical depth and electron temperature of τ = 2.5 − 5.3 (5.2 − 8) and
kT = 8 − 18 (7.5 − 14) keV , respectively, for a slab (spherical) geometry. The broadband SED is successfully modelled by
assuming either a standard accretion disc illuminated by a central X-ray source, or a thin disc with a slim disc emissivity profile.
The former model results in a black hole mass estimate of the order of 1010 M , slightly higher than prior optical estimates;
meanwhile, the latter model suggests a lower mass. Both models suggest sub-Eddington accretion when assuming a spinning
black hole, and a compact (∼ 10 rg ) X-ray corona. The measured intrinsic column density and the Eddington ratio strongly
suggest the presence of an outflow driven by radiation pressure. This is also supported by variation of absorption by an order of
magnitude over the period of ∼ 900 d .
Serendipitous discovery of an extended xray jet without a radio counterpart i...Sérgio Sacani
A recent Chandra observation of the nearby galaxy cluster Abell 585 has led to the discovery of
an extended X-ray jet associated with the high-redshift background quasar B3 0727+409, a luminous
radio source at redshift z = 2:5. This is one of only few examples of high-redshift X-ray jets known
to date. It has a clear extension of about 1200, corresponding to a projected length of 100 kpc, with
a possible hot spot located 3500 from the quasar. The archival high resolution VLA maps surprisingly
reveal no extended jet emission, except for one knot about 1:400 from the quasar. The high X-ray to
radio luminosity ratio for this source appears consistent with the / (1 + z)4 amplication expected
from the inverse Compton radiative model. This serendipitous discovery may signal the existence
of an entire population of similar systems with bright X-ray and faint radio jets at high redshift, a
selection bias which must be accounted for when drawing any conclusions about the redshift evolution
of jet properties and indeed about the cosmological evolution of supermassive black holes and active
galactic nuclei in general.
Radio continum emission_of_35_edge_on_galaxies_observed_with_the_vlaSérgio Sacani
Usando um dos maiores rádio observatórios do mundo, o Very Large Array do National Radio Astronomy, um grupo de astrônomos descobriram que os halos ao redor dos discos das galáxias espirais são muito mais comuns do que se pensava anteriormente.
A equipe, dirigida pela Dra. Judith Irwin, da Universidade de Queens, em Kingston, ON, Canadá, observou 35 galáxias espirais próximas de lado, de 11 a 137 milhões de anos-luz de distância da Terra.
As galáxias espirais, como a nossa própria Via Láctea ou a famosa Galáxia de Andrômeda, possuem uma vasta maioria de suas estrelas, gás, e poeira num disco plano em rotação com braços espirais. A maior parte da luz e das ondas de rádio observadas com telescópios veem de objetos localizados nesse disco.
“Nós sabíamos antes que alguns halos existiam, mas, usando o poder total do VLA atualizado e o poder total de algumas técnicas de processamento de imagens, nós descobrimos que esses halos são muito mais comuns entre as galáxias espirais do que nós pensávamos antes”, explicou a Dra. Irwin.
3D-Spatiotemporal forecasting the expansion of supernova shells using deep le...Sérgio Sacani
Supernova (SN) plays an important role in galaxy formation and evolution. In high-resolution galaxy simulations using massively
parallel computing, short integration time-steps for SNe are serious bottlenecks. This is an urgent issue that needs to be resolved
for future higher-resolution galaxy simulations. One possible solution would be to use the Hamiltonian splitting method, in
which regions requiring short time-steps are integrated separately from the entire system. To apply this method to the particles
affected by SNe in a smoothed particle hydrodynamics simulation, we need to detect the shape of the shell on and within which
such SN-affected particles reside during the subsequent global step in advance. In this paper, we develop a deep learning model,
3D-Memory In Memory (3D-MIM), to predict a shell expansion after a SN explosion. Trained on turbulent cloud simulations
with particle mass mgas = 1 M, the model accurately reproduces the anisotropic shell shape, where densities decrease by over
10 per cent by the explosion. We also demonstrate that the model properly predicts the shell radius in the uniform medium
beyond the training data set of inhomogeneous turbulent clouds. We conclude that our model enables the forecast of the shell
and its interior where SN-affected particles will be present.
A Comprehensive Theory for Neutron Star and Black Hole Kicks and Induced SpinsSérgio Sacani
Using twenty long-term 3D core-collapse supernova simulations, we find that lower compactness progenitors that explode quasi-spherically due to the short delay to explosion experience smaller neutron
star recoil kicks in the ∼100−200 km s−1
range, while higher compactness progenitors that explode
later and more aspherically leave neutron stars with kicks in the ∼300−1000 km s−1
range. In addition, we find that these two classes are correlated with the gravitational mass of the neutron star.
This correlation suggests that the survival of binary neutron star systems may in part be due to their
lower kick speeds. We also find a correlation of the kick with both the mass dipole of the ejecta
and the explosion energy. Furthermore, one channel of black hole birth leaves masses of ∼10 M⊙, is
not accompanied by a neutrino-driven explosion, and experiences small kicks. A second is through
a vigorous explosion that leaves behind a black hole with a mass of ∼3.0 M⊙ kicked to high speeds.
We find that the induced spins of nascent neutron stars range from seconds to ∼10 milliseconds and
that a spin/kick correlation for pulsars emerges naturally. We suggest that if an initial spin biases
the explosion direction, a spin/kick correlation is a common byproduct of the neutrino mechanism of
core-collapse supernovae. Finally, the induced spin in explosive black hole formation is likely large and
in the collapsar range. This new 3D model suite provides a greatly expanded perspective and appears
to explain some observed pulsar properties by default.
First identification of_direct_collapse_black_holes_candidates_in_the_early_u...Sérgio Sacani
The first black hole seeds, formed when the Universe was younger than ⇠ 500Myr, are recognized
to play an important role for the growth of early (z ⇠ 7) super-massive black holes.
While progresses have been made in understanding their formation and growth, their observational
signatures remain largely unexplored. As a result, no detection of such sources has been
confirmed so far. Supported by numerical simulations, we present a novel photometric method
to identify black hole seed candidates in deep multi-wavelength surveys.We predict that these
highly-obscured sources are characterized by a steep spectrum in the infrared (1.6−4.5μm),
i.e. by very red colors. The method selects the only 2 objects with a robust X-ray detection
found in the CANDELS/GOODS-S survey with a photometric redshift z & 6. Fitting their
infrared spectra only with a stellar component would require unrealistic star formation rates
(& 2000M# yr−1). To date, the selected objects represent the most promising black hole seed
candidates, possibly formed via the direct collapse black hole scenario, with predicted mass
> 105M#. While this result is based on the best photometric observations of high-z sources
available to date, additional progress is expected from spectroscopic and deeper X-ray data.
Upcoming observatories, like the JWST, will greatly expand the scope of this work.
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...Sérgio Sacani
The document discusses asymmetrical tidal tails observed around five open star clusters, which challenges Newtonian gravity. It summarizes how tidal tails form as stars escape clusters due to energy equipartition. Observations of the Hyades, Praesepe, Coma Berenices, COIN-Gaia 13, and NGC 752 clusters found more stars in the leading tidal tails within 50 pc of the clusters. Simulations show that in Newtonian gravity, tidal tails should be symmetrical, but asymmetries can arise in Milgromian dynamics. Future work is needed to better map tidal tails and develop Milgromian simulations.
Formation of low mass protostars and their circumstellar disksSérgio Sacani
Understanding circumstellar disks is of prime importance in astrophysics, however, their birth process remains poorly constrained due to observational and numerical challenges. Recent numerical works have shown that the small-scale physics, often wrapped into a sub-grid model, play a crucial role in disk formation and evolution. This calls for a combined approach in which both the protostar and circumstellar disk are studied in concert. Aims. We aim to elucidate the small scale physics and constrain sub-grid parameters commonly chosen in the literature by resolving the star-disk interaction. Methods. We carry out a set of very high resolution 3D radiative-hydrodynamics simulations that self-consistently describe the collapse of a turbulent dense molecular cloud core to stellar densities. We study the birth of the protostar, the circumstellar disk, and its early evolution (< 6 yr after protostellar formation). Results. Following the second gravitational collapse, the nascent protostar quickly reaches breakup velocity and sheds its surface material, thus forming a hot (∼ 103 K), dense, and highly flared circumstellar disk. The protostar is embedded within the disk, such that material can flow without crossing any shock fronts. The circumstellar disk mass quickly exceeds that of the protostar, and its kinematics are dominated by self-gravity. Accretion onto the disk is highly anisotropic, and accretion onto the protostar mainly occurs through material that slides on the disk surface. The polar mass flux is negligible in comparison. The radiative behavior also displays a strong anisotropy, as the polar accretion shock is shown to be supercritical whereas its equatorial counterpart is subcritical. We also f ind a remarkable convergence of our results with respect to initial conditions. Conclusions. These results reveal the structure and kinematics in the smallest spatial scales relevant to protostellar and circumstellar disk evolution. They can be used to describe accretion onto regions commonly described by sub-grid models in simulations studying larger scale physics.
Hydrogen Column Density Variability in a Sample of Local Compton-Thin AGNSérgio Sacani
We present the analysis of multiepoch observations of a set of 12 variable, Compton-thin, local (z<0.1) active galactic nuclei (AGN) selected from the 100-month BAT catalog. We analyze all available X-ray data from Chandra, XMMNewton, and NuSTAR, adding up to a total of 53 individual observations. This corresponds to between 3 and 7 observations per source, probing variability timescales between a few days and ∼ 20 yr. All sources have at least one NuSTAR observation, ensuring high-energy coverage, which allows us to disentangle the line-of-sight and reflection components in the X-ray spectra. For each source, we model all available spectra simultaneously, using the physical torus models MYTorus, borus02, and UXCLUMPY. The simultaneous fitting, along with the high-energy coverage, allows us to place tight constraints on torus parameters such as the torus covering factor, inclination angle, and torus average column density. We also estimate the line-of-sight column density (NH) for each individual observation. Within the 12 sources, we detect clear line-of-sight NH variability in 5, non-variability in 5, and for 2 of them it is not possible to fully disentangle intrinsic-luminosity and NH variability. We observe large differences between the average values of line-ofsight NH (or NH of the obscurer) and the average NH of the torus (or NH of the reflector), for each source, by a factor between ∼ 2 to > 100. This behavior, which suggests a physical disconnect between the absorber and the reflector, is more extreme in sources that present NH variability. NH-variable AGN also tend to present larger obscuration and broader cloud distributions than their non-variable counterparts. We observe that large changes in obscuration only occur at long timescales, and use this to place tentative lower limits on torus cloud sizes.
This paper analyzes NuSTAR X-ray observations of 9 optically selected type 2 quasars (QSO2s) at z < 0.5 that were candidates for being Compton-thick based on previous observations. Five new NuSTAR observations are reported. Five of the nine QSO2s were detected by NuSTAR in the 8-24 keV band, with three having sufficient counts for spectral modeling. For these three sources, NuSTAR data found their column densities were 2.5-1600 times higher and intrinsic luminosities were 10-70 times higher than previous estimates from Chandra and XMM-Newton alone. Accounting for these corrections, the authors estimate the Compton-thick fraction of optically selected type
Triple Spiral Arms of a Triple Protostar System Imaged in Molecular LinesSérgio Sacani
Most stars form in multiple-star systems. For a better understanding of their formation processes, it is important to
resolve the individual protostellar components and the surrounding envelope and disk material at the earliest
possible formation epoch, because the formation history can be lost in a few orbital timescales. Here we present
Atacama Large Millimeter/submillimeter Array observational results of a young multiple protostellar system,
IRAS 04239+2436, where three well-developed large spiral arms were detected in the shocked SO emission.
Along the most conspicuous arm, the accretion streamer was also detected in the SO2 emission. The observational
results are complemented by numerical magnetohydrodynamic simulations, where those large arms only appear in
magnetically weakened clouds. Numerical simulations also suggest that the large triple spiral arms are the result of
gravitational interactions between compact triple protostars and the turbulent infalling envelope.
M82 X-2 is the first pulsating ultraluminous X-ray source discovered. The luminosity of these extreme pulsars, if
isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but
with an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass
transfer rate can help discriminate between these two scenarios. In this paper, we follow the orbit of the neutron star
for 7 yr, measure the decay of the orbit (P P orb orb 8 10 yr 6 1 · » - - - ), and argue that this orbital decay is driven by
extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. If this is true,
the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also
strongly favors models where the accretor is a highly magnetized neutron star.
ALMA Observations of the Extraordinary Carina Pillars: A Complementary SampleSérgio Sacani
We present a study of six dusty and gaseous pillars (containing the HH 1004 and HH 1010 objects)
and globules (that contain the HH 666, HH 900, HH 1006, and HH 1066 objects) localized in the Carina
nebula using sensitive and high angular resolution (∼0.3′′) Atacama Large Millimeter/Sub-millimeter
Array (ALMA) observations. This is a more extensive study that the one presented in Cortes-Rangel
et al. (2020). As in this former study, we also analyzed the 1.3 mm continuum emission and C18O(2−1),
N2D+(3−2) and 12CO(2−1) spectral lines. These new observations revealed the molecular outflows
emanating from the pillars, the dusty envelopes+disks that are exciting them, and the extended HH
objects far from their respective pillars. We reveal that the masses of the disks+envelopes are in a
range of 0.02 to 0.38 M⊙, and those for the molecular outflows are of the order of 10−3 M⊙, which
suggests that their exciting sources might be low- or intermediate-mass protostars as already revealed
in recent studies at infrared and submillimeter bands. In the regions associated with the objects HH
900 and HH 1004, we report multiple millimeter continuum sources, from where several molecular
outflows emanate.
This document discusses the recycling of magnetic flux in the quiet Sun's corona. It presents a study that uses magnetogram observations to track photospheric magnetic flux fragments over time and models their evolution using a potential field approximation. The main findings are:
1) The quiet Sun's coronal flux is generally recycled on much shorter timescales, around 3 hours, than the corresponding recycling timescale of photospheric flux, which is around 8-19 hours.
2) When also considering emergence and cancellation of photospheric flux, the net replacement time of coronal flux is estimated to be only 1.4 hours.
3) The amount of magnetic reconnection driven by the motions and interactions of photospheric
A propable milli_parsec_supermassive_binary_black_hole_in_the_nearest_quasar_...Sérgio Sacani
Astrônomos usando o Telescópio Espacial Hubble da NASA descobriram que a Markarian 231 (Mrk 231), a galáxia mais próxima da Terra que abriga um quasar, é alimentada por dois buracos negros centrais girando violentamente um em relação ao outro.
A descoberta sugere que os quasares, os brilhantes núcleos das galáxias ativas, podem normalmente abrigar dois buracos negros centrais que caem, um na órbita do outro como resultado da fusão de duas galáxias. Como um par de patinadores, o buraco negro duplo gera uma tremenda quantidade de energia que faz o núcleo da galáxia que o abriga se sobrepor ao brilho da população de bilhões de estrelas da galáxia, que os cientistas então identificam como quasares.
Os cientistas procuraram nas observações de arquivo do Hubble feitas na radiação ultravioleta emitida do centro da Mrk 231 para descobrir o que eles descrevem como propriedades extremas e surpreendentes.
Similar to Continuum emission from within the plunging region of black hole discs (20)
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...Sérgio Sacani
The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy
was the construction of an observatory capable of characterizing habitable worlds. In this paper series
we explore the detectability of and interference from exomoons and exorings serendipitously observed
with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting
in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems
viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every
star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events
per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI)
lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive
the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable
with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain
detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet
features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm
water band where large moons can outshine their host planet, will aid in differentiating exomoon signals
from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin
to our Moon are more likely to be detected in younger systems, where shorter orbital periods and
favorable geometry enhance the probability and frequency of mutual events.
Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...Sérgio Sacani
Mars is a particularly attractive candidate among known astronomical objects
to potentially host life. Results from space exploration missions have provided
insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to
its toxicity. However, it can also provide potential benefits, such as producing
brines by deliquescence, like those thought to exist on present-day Mars. Here
we show perchlorate brines support folding and catalysis of functional RNAs,
while inactivating representative protein enzymes. Additionally, we show
perchlorate and other oxychlorine species enable ribozyme functions,
including homeostasis-like regulatory behavior and ribozyme-catalyzed
chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or
subsurface oxychlorine brines, and brines found in potential lifeforms, could
provide a unique niche for biomolecular evolution.
WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 RpSérgio Sacani
Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical
mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed
as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple
groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this
planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the
target set, demonstrating the outflow extends at least 5.8 × 105 km or 7.5 Rp This detection is significantly longer
than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is
blueshifted by −23 km s−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M⊕ Gyr−1
. Our
observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind.
However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or
differences in instrumental precision.
ANAMOLOUS SECONDARY GROWTH IN DICOT ROOTS.pptxRASHMI M G
Abnormal or anomalous secondary growth in plants. It defines secondary growth as an increase in plant girth due to vascular cambium or cork cambium. Anomalous secondary growth does not follow the normal pattern of a single vascular cambium producing xylem internally and phloem externally.
ESPP presentation to EU Waste Water Network, 4th June 2024 “EU policies driving nutrient removal and recycling
and the revised UWWTD (Urban Waste Water Treatment Directive)”
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptxMAGOTI ERNEST
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
Unlocking the mysteries of reproduction: Exploring fecundity and gonadosomati...AbdullaAlAsif1
The pygmy halfbeak Dermogenys colletei, is known for its viviparous nature, this presents an intriguing case of relatively low fecundity, raising questions about potential compensatory reproductive strategies employed by this species. Our study delves into the examination of fecundity and the Gonadosomatic Index (GSI) in the Pygmy Halfbeak, D. colletei (Meisner, 2001), an intriguing viviparous fish indigenous to Sarawak, Borneo. We hypothesize that the Pygmy halfbeak, D. colletei, may exhibit unique reproductive adaptations to offset its low fecundity, thus enhancing its survival and fitness. To address this, we conducted a comprehensive study utilizing 28 mature female specimens of D. colletei, carefully measuring fecundity and GSI to shed light on the reproductive adaptations of this species. Our findings reveal that D. colletei indeed exhibits low fecundity, with a mean of 16.76 ± 2.01, and a mean GSI of 12.83 ± 1.27, providing crucial insights into the reproductive mechanisms at play in this species. These results underscore the existence of unique reproductive strategies in D. colletei, enabling its adaptation and persistence in Borneo's diverse aquatic ecosystems, and call for further ecological research to elucidate these mechanisms. This study lends to a better understanding of viviparous fish in Borneo and contributes to the broader field of aquatic ecology, enhancing our knowledge of species adaptations to unique ecological challenges.
Comparing Evolved Extractive Text Summary Scores of Bidirectional Encoder Rep...University of Maribor
Slides from:
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Track: Artificial Intelligence
https://www.etran.rs/2024/en/home-english/
Travis Hills' Endeavors in Minnesota: Fostering Environmental and Economic Pr...Travis Hills MN
Travis Hills of Minnesota developed a method to convert waste into high-value dry fertilizer, significantly enriching soil quality. By providing farmers with a valuable resource derived from waste, Travis Hills helps enhance farm profitability while promoting environmental stewardship. Travis Hills' sustainable practices lead to cost savings and increased revenue for farmers by improving resource efficiency and reducing waste.
When I was asked to give a companion lecture in support of ‘The Philosophy of Science’ (https://shorturl.at/4pUXz) I decided not to walk through the detail of the many methodologies in order of use. Instead, I chose to employ a long standing, and ongoing, scientific development as an exemplar. And so, I chose the ever evolving story of Thermodynamics as a scientific investigation at its best.
Conducted over a period of >200 years, Thermodynamics R&D, and application, benefitted from the highest levels of professionalism, collaboration, and technical thoroughness. New layers of application, methodology, and practice were made possible by the progressive advance of technology. In turn, this has seen measurement and modelling accuracy continually improved at a micro and macro level.
Perhaps most importantly, Thermodynamics rapidly became a primary tool in the advance of applied science/engineering/technology, spanning micro-tech, to aerospace and cosmology. I can think of no better a story to illustrate the breadth of scientific methodologies and applications at their best.
What is greenhouse gasses and how many gasses are there to affect the Earth.moosaasad1975
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...Ana Luísa Pinho
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This presentation explores a brief idea about the structural and functional attributes of nucleotides, the structure and function of genetic materials along with the impact of UV rays and pH upon them.
2. Continuum emission from within the ISCO 367
MNRAS 531, 366–386 (2024)
magnetic stresses on the flow in the innermost disc regions. At the
time, the physical origin of the turbulent stress which drives accretion
was unknown.
We now know that magnetic fields are essential to driving accretion
in black hole discs, as accretion is mediated by angular momentum
transport driven by the magnetorotational instability (MRI; Balbus
Hawley 1991, 1998). It is therefore perhaps unsurprising that numeri-
cal simulations (e.g. Noble, Krolik Hawley 2010; Penna et al. 2010;
Zhu et al. 2012; Schnittman, Krolik Noble 2016; Lančová et al.
2019; Wielgus et al. 2022) generically find non-zero temperatures
at and within the ISCO, with non-zero associated thermal emission.
This emission will inevitably modify the SED of an observed black
hole disc, and may induce systematic errors in inferred black hole
properties.
The properties of the intra-ISCO thermal emission have previously
only been examined in a limited number of general relativistic
magnetohydrodynamic (GRMHD) simulations (e.g. Noble et al.
2011; Zhu et al. 2012; Schnittman et al. 2016). This analysis is
necessarily limited due to the great computational expense of running
GRMHD simulations, which prevents global parameter studies.
Recently, however, Mummery Balbus (2023) derived analytical
models for the intra-ISCO disc thermodynamics, using solutions
for the intra-ISCO kinematics of test particles (Mummery Balbus
2022). It was demonstrated in Mummery, Mori Balbus (2024a) that
these analytical solutions reproduce the liberated energy of the full
GRMHD simulations of Zhu et al. (2012), a result discussed in more
detail below. As such, it is now possible to derive continuum fitting
models which include analytic expressions for the locally liberated
energy within the ISCO, and examine the effects of this additional
emission on modelling of astrophysical sources. Presenting and
analysing such a continuum fitting model is the purpose of this paper.
While this work can in one sense be thought of as an extension
of classical models based on a new theoretical development, it
may in fact be more interesting to reverse this entire framework,
and seek to use observations of Galactic X-ray binaries to probe
a long-contentious question of theoretical physics. The vanishing
ISCO stress boundary condition has retained prominent advocates
(e.g. Paczyński 2000), who argue that a vanishing ISCO stress is a
natural consequence of viscous angular momentum transport.1
Even
if strictly true, in the notation of the remainder of this paper Paczyński
argues that the ISCO stress should scale as δJ ∼ α(H/r), where α
and H/r are the disc alpha parameter and aspect ratio respectively,
we shall argue however that even a per cent level ISCO stress can
have important observational implications (e.g. Fig. 1). Furthermore,
differing simulations have found measured values for the ISCO stress
which differ from each other by over an order of magnitude, and it
has been suggested that the initial magnetic field topology employed
in these simulations may play an important role in the ultimately
measured stress (e.g. Noble et al. 2010; Penna et al. 2010). It seems
likely that high quality X-ray observations of black hole discs will
contain signatures of the plunging region, much in the same way in
which they can be leveraged to constrain black hole properties. It is
the authors’ hope that the models developed in this paper, coupled
with future X-ray observations, may offer an observational handle
through which the complex physics of MHD turbulence in the inner
regions of black hole discs may be probed.
1It should be noted, of course, that angular momentum transport in an
accretion flow is fundamentally not governed by viscosity, but by MHD
turbulence which is a physically distinct process.
Figure 1. The radiative temperature profiles of post-processed GRMHD
simulations presented in Zhu et al. (2012) (black points; see the text),
compared to the analytical models developed in Mummery Balbus 2023,
Mummery et al. 2024a, blue curves) for three values of the black hole
spin (displayed on plot). Also shown are vanishing ISCO stress models for
comparison (red dashed curves). The simple analytical models reproduce
the results of full GRMHD simulations. The ISCO stress parameters are
δJ = 0.0055 for a• = 0.9, δJ = 0.0085 for a• = 0.7, and δJ = 0.007 for
a• = 0.
Indeed, observations of black hole systems are beginning to
hint at cracks in pre-existing theories. Fabian et al. (2020) argued
that observations of the X-ray binary system MAXI J1820 + 070
(hereafter MAXI J1820) in an extremely bright state could not
be successfully modelled without the addition of ad hoc thermal
emission components with small emitting areas and high emitting
temperatures. The characteristics of this additional emission were
argued to be similar to what might be expected from the intra-ISCO
fluid. Similar additional components were seen in another MAXI
source, MAXI J0637-430 (Lazar et al. 2021), and it is possible
that these components are wide spread but often ignored. Other
observations that may hint at the need for additional physics beyond
the standard approach include the extreme (beyond the Thorne 1974,
limit) spins inferred from continuum fitting of the high-mass X-ray
binary Cygnus X-1 (Zhao et al. 2021).
We will demonstrate in this paper that the guess put forward by
Fabian et al. (2020) was correct, and MAXI J1820 is extremely well
described by an accretion disc with a substantial emission component
stemming from within the ISCO. The addition of an intra-ISCO
component is required at a significance much stronger than 10σ,
with a change in χ2
statistic of χ2
= −630, −785, −820, −816,
respectively, for each of the four epochs of MAXI J1820 NuSTAR
data.
The remainder of this paper is organized as follows. In Sections 2–
4, we introduce the physics of the three components of the continuum
fitting model. In Section 2, we discuss the disc model, and how
the locally liberated disc energy is computed. In Section 3, we
discuss the orbits and energy shifts of photons emitted from disc
fluid within the ISCO. The physics of the radiative transfer of
the locally liberated energy are discussed in Section 4, where we
present the form of the rest-frame energy spectrum of the intra-ISCO
material. In Section 5, we show example X-ray spectra, computed
for a wide range of parameter space, highlighting the properties and
importance of the intra-ISCO emission. In Section 6, we show that
previously poorly fit X-ray spectra of MAXI J1820 are very well
described with the addition of intra-ISCO emission. A discussion
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3. 368 A. Mummery et al.
MNRAS 531, 366–386 (2024)
of the wider implications of these results is presented in Section 7,
before we conclude in Section 8. Some results are presented in a set
of Appendices.
2 THE DISC MODEL
The first key component of a continuum fitting model is a prescription
for the locally liberated energy of the disc. Typically, this locally
liberated energy is a function of disc location and a few global
physical free parameters of the system, such as the central black
hole’s mass and spin. In this work, we use the recent global thin
disc solutions of Mummery Balbus (2023). This model was then
extended in Mummery et al. (2024a) to better model the trans-ISCO
properties of the flow.
A detailed description of this new model is presented in these
recent papers, and we only briefly summarize the key results and
properties of them here (Appendix A contains a more detailed
discussion). On a fundamental level the model consists of the
classical Novikov Thorne (1973) description of the disc at radii
larger than the ISCO r rI. The Novikov Thorne (1973) model
is the basis for many contemporary continuum fitting models (e.g.
the KERRBB model in XSPEC Li et al. 2005). The vast majority
of previous continuum fitting models are curtailed at the ISCO (or
attempt to self-consistently compute the ISCO stress with an α-model
Straub et al. 2011, which is likely to be a severe oversimplification).
In our extended model, we solve for the fluid’s evolution interior to
the ISCO by assuming that the fluid elements undergo a geodesic
plunge, with thermodynamic evolution driven by a combination of
the radial stretching of the fluid (from the increasing intra-ISCO
radial velocity), and the vertical compression of the flow (driven
by the rapidly increasing vertical gravity of the flow as the event
horizon is approached). The disc fluid is assumed to remain optically
thick to scattering throughout the plunging region (an assumption
which can be tested, and is satisfied provided the accretion rate is not
too small ṁ ≡ Ṁ/Ṁedd 10−3
; see equation 16). The fact the flow
remains optically thick to scattering allows the local radiative flux to
be extracted from the disc’s thermodynamic quantities.
The joining of these two model solutions introduces an additional
free parameter to the disc system: the value of the ISCO stress,
denoted by δJ . Physically δJ corresponds to the angular momentum
the fluid passes back to the disc upon crossing the ISCO (normalized
by the angular momentum of a circular orbit at the ISCO), where
a value of δJ = 0 corresponds physically to no communication
between the disc and plunging region and a vanishing ISCO stress.
The value δJ = 1 represents maximal communication between the
two regions, and fluid elements cross the event horizon with zero
angular momentum.2
Numerical simulations (e.g. Shafee et al. 2008;
Noble et al. 2010) place δJ somewhere in the range δJ ∼ 0.02 − 0.2.
The success of this model in reproducing the properties of full
GRMHD simulations is displayed in Fig. 1, where we compare the
radiative temperature of these analytical models to those found in the
GRMHD simulations of Zhu et al. (2012). Zhu et al. (2012) extracted
a radiative temperature from the local cooling rate computed in the
2In principle, magnetic field lines which cross a spinning black hole and the
inner edge of the stable region of a disc can provide an external torque on the
disc, with photon emission sourced directly from the black hole’s spin-energy.
In this case, the parameter δJ represents the normalized angular momentum
flux of this process, not an internal fluid torque. For black hole spins a•
0.3594 all of the liberated energy of the disc can be sourced from this external
torque with no accretion required, and δJ can take any positive value (Agol
Krolik 2000).
GRMHD simulations run by Penna et al. (2010), and are displayed in
Fig. 1 by black dots, for three different black hole spins a = 0 (lower
panel), a = 0.7 (middle panel) and a = 0.9 (upper panel). The Zhu
et al. (2012) models all consist of an M = 10M black hole accreting
at roughly Ṁ ∼ 0.1Ṁedd. We take these parameters as input to the
analytical model. Various ‘effective’ α parameters are reported by
Zhu et al. (2012) and we take their values (α = 0.1 for a = 0.7
and a = 0.9, α = 0.01 for a = 0) for simplicity (Zhu et al. 2012,
their fig. 6). The one free parameter of the model is then the ISCO
parameters stress δJ . We overplot in Fig. 1 the vanishing ISCO stress
radiative temperature curve (red dashed curves), which are forced to
zero at the ISCO (contrary to the findings of the simulation), and in
blue (solid curves) the analytical model.
3 PHOTON ENERGY SHIFTS
The specific flux density Fν of the disc radiation, as observed by a
distant observer at rest (subscript ob), is given by
Fν(νob) =
“
S
Iν(νob) d ob. (1)
Here, νob is the photon frequency and Iν(νob) the specific intensity,
both measured at the location of the distant observer. We denote
by S the limits of this integral, which is to be taken over the entire
two-dimensional disc surface. The differential element of solid angle
subtended on the observer’s sky by the disc element is denoted d ob.
Since Iν/ν3
is a relativistic invariant (e.g. Misner, Thorne Wheeler
1973), we may write
Fν(νob) =
“
S
f 3
γ Iν(νem) d ob, (2)
where we define the photon energy shift factor fγ as the ratio of νob
to the emitted local rest frame frequency νem:
fγ (r, φ) ≡
νob
νem
=
pμUμ
(Ob)
pλUλ (Em)
=
U0
+
pφ
p0
Uφ
+
pr
p0
Ur
−1
, (3)
where (Ob) and (Em) refer to observer and emitter, respectively. The
covariant quantities pr, pφ, and −p0 (on the far right) correspond to
the radial momentum, angular momentum, and energy of the emitted
photon in the local (disc) rest frame. Note that pφ and −p0 may
be conveniently regarded as constants of the motion for a photon
propagating through the Kerr metric.
We will return to the properties of emitted spectrum in the disc rest
frame (Iν(νem)) in a later subsection, for now we focus our attention
on the photon energy shifts fγ .
The 4-velocity components of the disc fluid U0
, Uφ
, Ur
depend
only on radius. Outside of the ISCO, the fluid moves on approxi-
mately circular orbits, with 4-velocity components
Ur
= 0, (4)
Uφ
=
GM/r3
1 − 3rg/r + 2a
rg/r3
1/2
, (5)
U0
=
1 + a
rg/r3
1 − 3rg/r + 2a
rg/r3
1/2
, (6)
where rg ≡ GM/c2
is the black hole’s gravitational radius, M is
the black hole mass, and a is the black-hole spin parameter (with
dimensions of length). Within the ISCO the fluid is assumed to spiral
inwards while conserving its angular momentum and energy, which
results in (Mummery Balbus 2022)
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4. Continuum emission from within the ISCO 369
MNRAS 531, 366–386 (2024)
Ur
= −c
2rg
3rI
rI
r
− 1
3/2
, (7)
Uφ
=
2rgγ ac + J(r − 2rg)
r(r2 − 2rgr + a2)
, (8)
U0
=
γ c(r3
+ ra2
+ 2rga2
) − 2Jrga
rc(r2 − 2rgr + a2)
, (9)
where we denote by rI the ISCO radius. In these final two expressions,
the constants of motion J and γ represent the specific angular
momentum and energy of the ISCO circular orbit respectively, and
are equal to (Mummery Balbus 2022)
J = 2
√
3rgc
1 −
2a
3
√
rgrI
, (10)
γ =
1 −
2rg
3rI
. (11)
Starting from a finely spaced grid of points described by Cartesian
impact parameters (α, β) in the image plane, we trace the geodesics
of each photon back to the disc plane, recording (rf, pr, pφ, p0)
for each photon. We use the code YNOGK (Yang Wang 2013),
which is based on GEOKERR (Dexter Agol 2009), to numerically
solve for the photon geodesics (see Ingram et al. 2019, for a more
detailed description of the grid used). The parameter rf is the radius at
which the photon crosses the θ = π/2 disc equatorial plane. Together
these parameters uniquely determine the energy-shift factor fγ . The
differential element of solid angle subtended by the disc surface is
simply d ob = dαdβ/D2
, for an observer at a distance D from the
disc.
As an interesting first example, we plot in Fig. 2 the energy shift
factor fγ as observed in the image plane, fγ (α, β). This figure was
produced for a Schwarzschild black hole a = 0, observed at θobs =
85◦
. Note also the pronounced gravitational lensing of the near-
ISCO region. The colour bar denotes the energy shift, while the
white curve corresponds to photons emitted from precisely the ISCO
radius. An extremely interesting, and potentially surprising, result
is that the observed photon energy-shift actually peaks within the
ISCO, for these system parameters (see the lower panel of Fig. 2
for a zoom-in of the intra-ISCO region). This result is simple to
understand qualitatively, as the fluid flow within the ISCO retains a
strong azimuthal character, and is not moving on a purely ‘radial’
plunge.
To understand this further, in Fig. 3 we plot quasi-Cartesian
velocity streamlines of the disc fluid both within and outside of
the ISCO. We define quasi-Cartesian coordinates
X = r cos(φ), Y = r sin(φ), (12)
with corresponding dimensionless velocities
βX =
1
c
dX
dτ
=
1
c
Ur
cos(φ) − rUφ
sin(φ) , (13)
βY =
1
c
dY
dτ
=
1
c
Ur
sin(φ) + rUφ
cos(φ) . (14)
These velocities define streamlines of the flow. It is clear to see in
Fig. 3 that the fluid flow retains a strong azimuthal character, even
within the ISCO (denoted by a black dashed curve). The magnitude of
the velocity itself increases within the ISCO, such that large Doppler
boosting can overcome the increasing gravitational redshift of the
near horizon spacetime. This leads to an increase in the photon
energy shifts within the ISCO for inclined disc systems (e.g. those
shown in Fig. 2).
Figure 2. Upper: An image plane view of the photon energy shift factor for a
disc system about a Schwarzschild black hole a = 0, observed at θobs = 85◦.
This figure also highlights the pronounced gravitational lensing of the near-
ISCO region. The colour bar denotes the energy shift factor of the photons
emitted from a given disc region and observed in the image plane at (α,
β). The white curve corresponds to the image plane location of the ISCO.
The observed photon energy-shift actually peaks within the ISCO, for these
system parameters. Lower: A zoom-in of the region within the ISCO.
The relative importance of the different effects of Doppler and
gravitational energy shifting depend predominantly on the inclination
of the disc system. In Fig. 4, we plot Schwarzschild photon energy
shift maps for inclinations of 60◦
(upper panel) and 30◦
(lower panel).
Photons emitted from within the ISCO may still be blue-shifted
for more moderately inclined systems (upper panel, Fig. 4), but
more face-on discs are dominated by the gravitational red-shift, and
photons emitted from within the ISCO reach the observer at lower
energies (lower panel, Fig. 4).
Photon energy shift maps for the Kerr metric with general
spin parameter a all show qualitatively similar behaviour to the
Schwarzschild metric displayed explicitly here, and are not shown
explicitly.
Finally, we note that we have set up the calculation here in such
a way that only those photons which escape to infinity contribute
to the observed flux. This is important as within the ISCO fluid
elements pick up a large velocity component in the direction of
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5. 370 A. Mummery et al.
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Figure 3. Quasi-Cartesian velocity streamlines of the disc fluid both within
and outside of the ISCO. For this figure, we take a = 0, and denote by a black
dashed line the location of the ISCO. The colour bar displays the value of β,
where β2 ≡ β2
X + β2
Y , where βX and βY are defined in the text. Note that β
1 for some radii, this is not unphysical, as neither X nor Y correspond to
physical proper distances. The velocity field of the disc fluid is still dominated
by predominantly azimuthal motion, even within the ISCO.
the black hole’s event horizon. A sizeable fraction of the photons
emitted by a fluid element which is emitting isotropically in its own
rest frame will be beamed into the black hole in the ‘lab’ frame.
While this beaming is taken into account in our calculations, we do
not explicitly calculate the ratio of captured-to-escaped photons. We
direct the reader interested in this effect to Agol Krolik (2000),
who calculated the captured-photon fraction for discs with a finite
ISCO stress (but no intra-ISCO emission).
4 PHOTON STARVATION: RADIATIVE
TRANSFER INSIDE THE ISCO
The disc fluid within the ISCO remains optically thick to scattering
right down to the event horizon of the black hole, a result which holds
provided that the Eddington-normalized accretion rate of the disc is
moderate. To see this, combine the definition of the scattering optical
depth τscat = κes, with the constraints of mass conservation Ṁ =
2πrUr
, and the rapid radial acceleration of the intra-ISCO region,
which leads to a radial velocity Ur
= c 2rg(rI − r+)3/3rI r3
+ as the
fluid approaches the event horizon r → r+ (see equation 7). The
minimum scattering optical depth is therefore
τscat,min =
κesṀc
2πGM
3rI r+rg
2(rI − r+)3
, (15)
and upon substituting for Ṁ = ṁṀedd = ṁLedd/(ηc2
), with Edding-
ton luminosity Ledd = 4πGMc/κes, leaves the simplified result (ṁ
is the Eddington-normalized accretion rate, η is the mass-to-light
accretion efficiency)
τscat,min =
ṁ
η
6rI r+rg
(rI − r+)3
. (16)
The remaining factors are all order unity for low spins, and we see that
we have optically thick (to scattering) fluid down to the event horizon
provided ṁ η. This result highlights the fact that while there is a
Figure 4. An image plane view of the photon energy shift factor for a black
hole disc system about a Schwarzschild black hole a = 0, observed at θobs =
60◦ (upper) and θobs = 30◦ (lower). The colour bar denotes the energy shift
factor of the photons emitted from a given disc region and observed in the
image plane at (α, β). The white curve corresponds to the image plane location
of the ISCO.
substantial drop in the density across the plunging region, the density
required to maintain a substantial Eddington ratio is sufficiently high
that this drop does not lead to optically thin (to scattering) material
in the plunging region.
Photons travelling through a material which is optically thick
to scattering will in general thermalize their energy. However, the
energy liberated from the disc fluid can only be carried out as purely
thermal photon emission as long as there are a sufficient number
of photons to carry away the total energy budget with the energy
distribution prescribed by the blackbody spectral profile. If there
are an insufficient total number of photons available, each emitted
photon will have to carry a (potentially significantly) larger energy,
so that the total energy budget can be radiated away. The number
density of photons required to carry away the energy budget of a
blackbody at temperature T is nγ ∝ T3
and therefore, for the nearly
isothermal effective temperature profiles we find for the intra-ISCO
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6. Continuum emission from within the ISCO 371
MNRAS 531, 366–386 (2024)
region (Fig. 1), this corresponds to a roughly constant requirement
of photon number density throughout the plunging region.
However, while intra-ISCO flows require a near constant number
density of photons, the availability of photons rapidly decreases
across the ISCO. This is because photons are produced by free-
free processes, the emissivity (energy produced per unit volume per
unit time) of which (ηff) depends on the square of the disc density
ηff = η0 m−2
p T 1/2
c ρ2
, (17)
where η0 1.4 × 10−27
erg s−1
cm−3
caries the dimensions of
ηff, mp is the protons mass, and Tc and ρ are the disc fluids central
temperature and density respectively (and should take dimensionless
values appropriate for the cgs units system). The density of the disc
fluid ρ /H drops rapidly across the intra-ISCO region, owing to
the constraint of a constant radial mass flux Ṁ = 2πrUr
, coupled
with a rapidly growing radial velocity Ur
. Therefore, as the disc fluid
is accelerated over the ISCO, it quickly loses the ability to produce the
required number of photons to maintain a thermal emission profile.
A fluid which is unable to produce sufficient photons to radiate away
all of its energy budget as a thermal spectrum is said to be ‘photon
starved’. Intra-ISCO emission is photon-starved, and will therefore
be characterized by extreme ‘spectral hardening’.
It is possible to derive a critical curve in disc parameter space that
demarcates the approximate transition from ‘normal’ to ‘extreme’
spectral hardening. The flux (energy per unit area per unit time) of
photons produced by free–free processes across the disc atmosphere
is approximately ηffH, and if this becomes lower than the flux
required to be carried away for thermal emission, or explicitly when
ηffH σT 4
, (18)
there will be an insufficient photon number density in the flow
and each photon must carry a larger energy to radiate away the
disc energy budget.3
Using standard disc scaling laws Davis El-
Abd (2019) showed that extreme spectral hardening occurs for disc
systems which cross the critical curve
log10 Qcrit = log10 Q0 + 7.5 log10 T − 2.125 log10 , (19)
where all discs with Q ࣠ Qcrit will show extreme hardening. The
parameter Q0 depends only on fundamental constants
Q0 ≡
m2
p κ7/8
es σ2
η0 c
, (20)
and Q is the vertical gravity of the black hole experienced by the disc
fluid which is defined through the equation of vertical hydrostatic
equilibrium4
−
dP
dz
= ρQz, (21)
where P and ρ are the total pressure and density of the fluid,
respectively, and z is the vertical coordinate. In the Kerr metric Q is
given by (Abramowicz, Lanza Percival 1997)
Q =
GM•
r3
Rz(r, a•), (22)
3We assume here that during the time taken for photons to traverse the disc
atmosphere H a negligible amount of energy is advected into the black hole.
This is a reasonable assumption for thin discs as the vertical diffusion time
t ∼ Hτ/c ∼ HκṀ/rUr shrinks by the same factor with which the fluid’s
radial velocity grows, and H is small compared to r.
4This is somewhat of a misnomer, as Q depends on the four-momentum of
the orbiting disc fluid as well as the properties of the central black hole.
Figure 5. Phase space (Q, T, ) plots of the thin disc solutions displayed
in Fig. 1 (thick curve), and the ‘critical curve’ of extreme spectral hardening
described in Davis El-Abd 2019 (thin curve). Points above the critical
curve (at the same surface density, displayed by the colour bar) will display
normal spectral hardening, while points below the curve will show extreme
hardening. The transition point of both solutions is very close to the ISCO
(red star). Intra-ISCO fluid can be identified by smaller surface densities, and
larger vertical gravity.
where Rz is a (dimensionless) relativistic correction term (listed in
Appendix A).
For typical disc parameters, the transition to extreme spectral
hardening occurs almost precisely at the ISCO radius. This can be
seen in Fig. 5, where we plot the vertical gravity Q against the
effective temperature of the disc, for the analytical disc solutions
which reproduce the Zhu et al. (2012) GRMHD simulation results
(i.e. those profiles displayed in Fig. 1). We also display the Davis
El-Abd (2019) critical curve (i.e. equation (19)), with T and
computed at each radius in the disc. Regions of the disc (at fixed
surface density, denoted by the colour of the plot) that are above
the critical curve display ‘normal’ spectral hardening, while regions
of the disc below the critical curve will show extreme spectral
hardening. As is clear to see in Fig. 5, the interception point between
the disc profile and the critical curve is almost exactly the ISCO
radius (denoted by a red star in Fig. 5). This means that the emission
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7. 372 A. Mummery et al.
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Figure 6. The X-ray spectra computed from TLUSTY post-processing of
GRMHD simulations (Zhu et al. 2012, black points), compared to the colour-
corrected analytical models developed here (green solid curve). The effective
temperature profiles are those displayed in Fig. 1, and the colour-correction
parameters are fI = 4, ξ = 6 (a• = 0.9), and fI = 3, ξ = 4 (a• = 0.7).
sourced from within the ISCO will be observed to be significantly
hardened compared to the emission sourced from the main body of
the disc.
This behaviour was observed in Zhu et al. (2012), where the local
TLUSTY spectra (e.g. Hubeny Lanz 1995; Davis Hubeny 2006;
Davis, Done Blaes 2006) sourced from the intra-ISCO region
(i.e. spectra post-processed from the Penna et al. 2010; GRMHD
simulations) peaked (in the source rest frame) at energies up to Eγ
∼ 100 keV, despite the effective temperature of the flow being at
significantly lower energies kT ∼ 1−10 keV (see Fig. 6).
Spectral hardening in the continuum fitting community is normally
modelled with a single spectral hardening factor fcol ≥ 1, which
modifies the locally emitted spectrum from thermal in the following
simple manner
Iν(νem) =
1
fcol
4
Bν(νem, fcolT ), (23)
where Bν is the usual Planck function. Note that the normalization
factor of f −4
col means that the total luminosity of the emitted photons
is unchanged by spectral hardening (and therefore total energy is
conserved), but that typical photons are emitted with a larger energy
hν ∼ fcolkT ≥ kT.
It is not immediately clear that the complex physics of photon
starvation (captured by the full TLUSTY calculations) will be in any
way well described by a simple colour-corrected blackbody model.
We do however have a well-defined test case to probe this physics, as
the Zhu et al. (2012) spectra are generated from effective temperature
profiles which we know are well described by the analytical disc
models of Mummery Balbus (2023). Therefore, if we are able to
reproduce in detail the observed spectra of Zhu et al. (2012), then the
simple colour-corrected emission model must be capturing the full
physics of the TLUSTY radiative transfer calculations.
We experimented numerically with a number of colour-correction
prescriptions for the photon starved intra-ISCO region. A single
constant fcol = fI 1 did a reasonable job at reproducing the Zhu
et al. (2012) disc spectra, but the following functional form
fcol = fI
r
rI
−ξ
, r ≤ rI , (24)
where fI ≥ 1 and ξ ≥ 0 are constant fitting parameters, did an
excellent job. We will henceforth refer to ξ as the ‘photon starvation
parameter’. We display in Fig. 6 X-ray spectra generated using the
above prescription, and the disc effective temperature profiles of
Fig. 1, compared to the TLUSTY spectra generated from temperature
profiles extracted from GRMHD simulations, presented in Zhu et al.
(2012). The simple models presented in this paper do a remarkable
job at reproducing the complex physics of post-processed GRMHD
simulations.
In Fig. 6, we split the individual contributions to the total X-ray
spectrum (green solid curve) into disc regions exterior to the ISCO
(red dot–dashed) and interior to the ISCO (orange dashed). While the
bulk of the total luminosity originates from extra-ISCO disc regions,
above Eγ ∼ 10 keV the emission is entirely dominated by emission
sourced from within the ISCO.
Naturally, a tuneable colour-correction still represents a significant
simplification of the full radiative transfer of the intra-ISCO region.
In a future analysis, we wish to explore the physical properties of the
radiative transfer within the ISCO in significantly more detail, and it
seems likely that this prescription can be improved upon. However,
existing tools such as TLUSTY are liable to crash in the particular
region of parameter space relevant for intra-ISCO accretion (see e.g.
Zhu et al. 2012; Davis El-Abd 2019, for a discussion of this), and
developing new radiative transfer tools lies beyond the scope of this
current paper. While this treatment may need to be revisited in future
studies, it is clear that this modelling does capture the physics of
the plunging region (Fig. 6). In its current form, this model offers a
route to analysing intra-ISCO emission in X-ray binaries, which is a
valuable addition.
Finally, it is worth noting that TLUSTY itself has a number of
simplifying assumptions which may not be formally valid within
the ISCO. First, TLUSTY assumes that the disc electrons obey a
thermal distribution (with a single temperature identical to the
ion temperature). Hankla, Scepi Dexter (2022) have recently
argued that this assumption might break down, and the intra-ISCO
electron population may in fact be better described by a non-thermal
distribution. In addition, TLUSTY neglects irradiation of the disc
atmosphere from above, and within the ISCO self-irradiation is likely
to be important at small radii. Models developed for post-processing
GRMHD simulations (e.g. Narayan et al. 2016; Kinch et al. 2021)
include these effects, and in principle, a future extension of these
models should include these effects.
5 EXAMPLE X-RAY SPECTRA
Fig. 6 highlights the main observational effect of including intra-
ISCO emission, namely the appearance of an additional hot and
small (compared to the main body of the disc) quasi-blackbody
component and a weak and soft power-law tail extending to much
higher energies. In this section, we examine these properties in more
detail.
There are of course two different modifications to the disc emission
which occur when a disc has a non-zero ISCO stress. The first results
simply from additional flux sourced from the stable disc regions (r
rI) that escapes to the observer (e.g. Agol Krolik 2000), while
in this paper we will focus on the extra emission sourced from within
the ISCO.
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8. Continuum emission from within the ISCO 373
MNRAS 531, 366–386 (2024)
Figure 7. The different spectral effects of modifying the vanishing ISCO
stress boundary condition. The extra emission from a disc with a finite ISCO
stress comes in two main components. Additional emission from the main
body of the disc (outside of the ISCO) simply hardens the main disc spectrum
(contrast the red dot–dashed and black dashed spectra). In contrast, the intra-
ISCO emission typically presents itself as an additional hot and small quasi-
blackbody component (orange dashed curve). For physical parameter values,
see the main body of the text.
In Fig. 7, we highlight the different properties of these two
additional emission components. Each X-ray spectrum is produced
assuming a M = 10 M black hole, which is not rotating (a• = 0),
and is fed by a constant mass accretion rate Ṁ = Ledd/c2
, where
Ledd = 1.26 × 1038
(M/M) erg s−1
(this corresponds to a bolometric
disc luminosity of L ∼ 0.1Ledd, typical for soft-state X-ray binaries).
The disc is observed at an inclination of i = 45◦
. For simplicity, we
take a colour-correction factor in the main body of the disc of fd =
1.7, a value we also take for fI. We take ξ = 2, similar to the value
found from fits to MAXI J1820 discussed later.
In red (dot–dashed), we show the X-ray spectrum that would be
observed if the disc had a vanishing ISCO stress (δJ = 0). In black
(dashed), we show the spectrum observed from the disc assuming a
non-zero ISCO stress δJ = 0.05, but still with no emission sourced
from within the ISCO. The inclusion of this additional extra-ISCO
emission simply hardens the disc spectrum slightly, and is in general
degenerate with a change in Ṁ or source-observer distance (Li et al.
2005). However, when emission within the ISCO is included (blue
solid curve), we see that intra-ISCO emission has a different character
to extra-ISCO emission, and in general dominates over all other
emission regions for moderately high photon energies E ∼ 5 keV.
The emission sourced from within the ISCO is displayed by an
orange dotted curve, and is reasonably well described by a single
temperature blackbody. The physical origin of this quasi-single-
temperature appearance is chiefly related to the interplay between the
rising colour-temperature of the flow (e.g. Fig. 1) being counteracted
by the rising gravitational redshifting of the emitted photons (e.g.
Fig. 4) of this region. This leads to only a small region from within
the ISCO contributing the majority of the additional flux.
It is clear to see from Fig. 7 that a non-zero ISCO stress increases
the radiative efficiency of a black hole accretion flow, typically
defined as η ≡ L/Ṁc2
. This result is well known, and in fact the
ISCO stress can itself be parametrized entirely as an additional
accretion efficiency η (see Agol Krolik 2000, who do not include
emission from within the ISCO in their calculation). As can be seen
in Fig. 7, the extra emission from within the ISCO represents a
Figure 8. The effect of varying the disc’s ISCO stress parameter on the
emergent X-ray spectrum. As the ISCO stress is increased there is a small
increase in emission from outside of the ISCO (contrast the dashed curves
with the red dot–dashed vanishing ISCO stress curve), but the principle
modification is the increasing flux from the intra-ISCO region. Increasing
the ISCO stress dramatically increases both the ‘temperature’ and ‘emitting
area’ of the emission within the ISCO (dotted curves). All non-displayed
parameters are identical to those in Fig. 7.
small fraction of the total emitted luminosity (as has been argued
previously, e.g. Zhu et al. 2012), but it represents a huge increase in
the flux at certain observed frequencies. We will demonstrate in the
following section that this is of crucial observational significance.
Thermal emission sourced from within the ISCO is particularly
sensitive to four free parameters, the ISCO stress δJ , the photon
starvation parameter ξ, the disc-observer inclination i and the black
hole spin a•. We now examine the effects of each of these parameters
in turn, keeping to the same figure conventions: vanishing ISCO stress
discs are shown by dot–dashed curves, finite ISCO stress discs with
no intra-ISCO emission by dashed curves, the emission from within
the ISCO is shown by dotted curves and the total disc flux is shown
by a solid curve. All parameters (except when explicitly stated) are
the same as those used in Fig. 7.
The most obvious parameter on which the intra-ISCO emission
depends is the ISCO stress parameter δJ . In Fig. 8, we display the
effect of varying this parameter on the X-ray spectrum observed
at i = 45◦
. For low ISCO stress values (e.g. values much lower
than is seen in GRMHD simulations Noble et al. 2010; Schnittman
et al. 2016), the X-ray spectrum looks near indistinguishable from a
vanishing ISCO stress disc, and the intra-ISCO emission is that of
a cool and very small blackbody (light blue curve). However, as the
ISCO stress is increased the intra-ISCO emission gets both hotter and
larger in amplitude (it has a larger ‘emitting area’ in the language
of a blackbody profile). This can be clearly seen from observing
the dotted profiles (Fig. 8) growing in importance and ultimately
dominating the high energy emission for δJ 0.03.
It is extremely important to stress that the intra-ISCO emission
is much more sensitive to δJ than the additional emission sourced
from finite ISCO stress discs from r ≥ rI. This can be seen most
clearly in Fig. 8, as the finite ISCO stress discs (dashed curves) show
a moderate range of behaviours for increasing δJ , while the intra-
ISCO emission (dotted curves) shows a much stronger dependence.
This means that accounting for the impact of deviations from a no-
torque boundary condition is even more important for obtaining a
robust spin estimate than previously models concluded (e.g. a simple
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Figure 9. The effect of varying the intra-ISCO photon starvation parameter
ξ on the emergent X-ray spectrum. When ξ ࣠ 3 the intra-ISCO emission is
well described by additional quasi-blackbody emission, while for even harder
emission the additional spectrum becomes more power-law like.
change in Ṁ cannot mimic intra-ISCO emission, although it can
mimic the extra emission sourced from exterior to the ISCO which
results from a non-zero stress; Li et al. 2005). These degeneracies
will be examined in more detail in a follow-up work.
The precise observed form of the intra-ISCO emission depends on
how extreme the photon starvation becomes within the ISCO. This
can be seen in Fig. 9. In Fig. 9, we show X-ray spectra (produced
with otherwise identical parameters to the models discussed above),
but with different values of the starvation parameter ξ. For values ξ
࣠ 3, the intra-ISCO emission is observed to have a quasi-blackbody
form; however, if ξ reaches values larger than this then the observed
emission becomes increasingly well approximated by a power law.
As we discussed in Section 4, the precise physics of the radiative
transfer within the ISCO is uncertain, and will need to be addressed
with dedicated calculations. It appears that intra-ISCO emission is
best approximated by a hot-and-small blackbody, as strong power-
law tails require extremely large colour-corrections (of order f
100), and even large colour-corrections (like the ξ = 3 case) show
quasi-thermal emission. We do note however that there is sufficient
energy liberated within the ISCO to power pronounced power-law
components. We stress that this ‘power law’ appears from a sum
of blackbodies, each with a progressively higher colour correction,
and not any intrinsic change in the modelling of the emission
(a similar effect produces a power-law spectrum from thermal
Comptonization).
Finally, in Figs 10 and 11 we examine the effect of varying the
disc-observer inclination and black hole spin on the emergent flux
sourced from within the ISCO. In each figure, the upper panel shows a
vanishing ISCO stress disc spectrum, the middle panel the spectrum
resulting from a disc with a finite ISCO stress and no intra-ISCO
emission, while the lowest panel shows the full disc model, with
intra-ISCO emission displayed as a dotted curve.
In Fig. 10, we display X-ray spectra observed at different incli-
nations (displayed in figure legend). For these Schwarzschild discs,
the intra-ISCO emission is always important at energies E 10 keV.
The emission from within the ISCO grows with importance with
increasing inclination, a result of Doppler beaming of the inner disc
(see e.g. Fig. 2 and the discussion of Section 3). The intra-ISCO
disc region can produce the majority of the flux above E ∼ 5 keV
Figure 10. The effect of varying the disc-observer inclination on the prop-
erties of the emission sourced from within the ISCO. For the Schwarzschild
black holes considered in this figure, the intra-ISCO emission is always
important at energies E 10 keV. The emission from within the ISCO grows
with importance with increasing inclination, a result of Doppler beaming of
the inner disc (see e.g. Fig. 2). The intra-ISCO disc region can produce the
majority of the flux above E ∼ 5 keV for moderate inclinations i 60◦.
Upper panel: vanishing ISCO stress discs; middle panel: discs with a finite
ISCO stress and no intra-ISCO emission; lower panel: the full disc model,
with intra-ISCO emission displayed as a dotted curve.
Figure 11. The effect of varying the black hole spin parameter a• on the
X-ray spectrum, and the properties of the emission sourced from within the
ISCO. Intra-ISCO emission is most important at lower black hole spins, a
result simply of the larger event horizon-to-ISCO radial range at low spins.
With intra-ISCO emission included, the differences between different spin
parameters are less pronounced. Upper panel: vanishing ISCO stress discs;
middle panel: discs with a finite ISCO stress and no intra-ISCO emission;
lower panel: the full disc model, with intra-ISCO emission displayed as a
dotted curve.
for moderate inclinations i 60◦
. While the differences between
the extra-ISCO emission of finite and vanishing ISCO stress discs
show a weak dependence on inclination, the dependence of the intra-
ISCO emission on inclination is much stronger. This suggests that
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disc models which include intra-ISCO emission may provide tighter
constraints on source-observer inclinations.
Finally, in Fig. 11 we display the effects of varying the black
hole spin parameter a• on the intra-ISCO emission. Perhaps un-
surprisingly, intra-ISCO emission is most important at lower black
hole spins, a result simply of the larger event horizon-to-ISCO
radial range of low spin spacetimes. Interestingly, the intra-ISCO
emission (for those physical parameters given by those of Fig. 7)
is relatively insensitive to black hole spin (see the dotted curves
in Fig. 11), with each quasi-blackbody component having roughly
similar temperature and area. This stops being true at the very highest
spins (orange curves), where the effective area is strongly suppressed.
It is interesting, and important, to note that with the inclusion
of intra-ISCO emission, the differences between X-ray spectra
produced by black holes with different spin parameters becomes
less pronounced. This property will have relevance for the ability of
continuum fitting to place constraints on black hole spins.
To summarize, intra-ISCO emission is always important, but is
particularly important for black holes with low spin parameters
(Fig. 11). The emission from within the ISCO is characterized by a
hot-and-small quasi-blackbody profile, which grows in prominence
for larger ISCO stress parameters (Fig. 8) and inclinations (Fig. 10).
For large values of the photon starvation parameter ξ the intra-
ISCO emission instead appears as a power-law component (sourced
from a sum of blackbodies with rapidly growing colour correction),
but further study is required to determine whether this level of
photon starvation is applicable to real systems (Fig. 9). If this
level of spectral hardening is relevant then there is sufficient energy
liberated within the ISCO to power a possibly substantial power-law
fraction.
Finally, we discuss some apparent discrepancies between the
results of this section and the results of Zhu et al. (2012). Zhu
et al. (2012) argue that their Schwarzschild simulations showed
the smallest difference to standard vanishing ISCO stress models –
while we have argued that a large intra-ISCO area should maximize
the discrepancy. It is important to stress that Zhu et al. (2012)
were principally concerned with potential degeneracies in black
hole spin measurements in models with and without intra-ISCO
emission, while we are concerned with the more general features
of the spectrum. Most important however is that we have explored
how the spectrum varies as black hole spin is changed whilst δJ and
ξ are held constant. In the particular case of the Zhu et al. (2012)
analysis however, the Schwarzschild simulation showed substantially
lower spectral hardening (see e.g. their Fig. 9), suggesting a decrease
in ξ with lower spin. We caution against reading too much into
this scaling however, other simulations (e.g. Noble et al. 2011,
which are somewhat better resolved) find much larger discrepancies
between simulations of Schwarzschild discs and standard vanishing
ISCO stress models. In addition, both of the Zhu et al. (2012)
and Noble et al. (2010) simulations use cooling functions, while
modern numerical methods solve the full equations of radiation
hydrodynamics. Future comparisons of the models presented here
and modern simulations is of great interest.
Finally, we again stress the general philosophy of the approach
put forward in this paper – which is that observations may have a
lot to teach us about intra-ISCO accretion, particularly in the most
theoretically uncertain regions of parameter space, such as what
the expected values of δJ and ξ are as a function of other system
parameters. While it is an important bench-marking test that the
models developed in this paper can reproduce the thermodynamic
(Fig. 1) and observed (Fig. 6) properties of individual GRMHD
simulations, modelling of observations should be allowed to stand
alone and at some level inform theoretical understanding of this
region.
6 EMISSION FROM WITHIN THE ISCO OF
MAXI J1820
With the properties of the intra-ISCO continuum emission now
discussed, we proceed by analysing the X-ray spectrum of the low
mass black hole X-ray binary MAXI J1820 (Kawamuro et al. 2018;
Tucker et al. 2018) taken during an outburst in 2018 (Shidatsu et al.
2019). This thermal-dominated X-ray spectrum has previously been
modelled by Fabian et al. (2020), who found that they were unable to
describe the soft-state spectrum of MAXI J1820 with conventional
disc models (e.g. Li et al. 2005), owing to the presence of additional
hot-and-small thermal emission. Fabian et al. (2020) speculated that
this additional emission may be sourced from within the ISCO, and as
such this is an ideal observation with which to test the new accretion
model developed in this paper.
A representative X-ray spectrum is shown in Fig. 12, in black
we display the data, which is taken from the NuSTAR observation
Nu29 (different NuSTAR observations are distinguished by the last
two digits in their OBSIDs; we refer the reader to Fabian et al.
2020, for details on the individual observations). We observe a clear
thermal continuum and a high energy power-law tail (presumably
produced by the Compton up-scattering of seed disc photons by a
hot electron corona). In the upper left panel we show a best fit of
kerrbb + cutoffpl5
to the data. As we are not interested in
the best fitting parameters of the kerrbb fit, merely in its overall
performance, we allow all parameters (except the source-observer
distance which we fix to 3 kpc, and the ISCO stress which we
fix to 0) to freely vary during the fit. We do not report the best
fitting kerrbb parameters, as the fit is so poor (see also Fabian
et al. 2020). In the canonical picture, kerrbb should well describe
the thermal continuum, with cutoffpl modelling the power-law
tail. The total fitted model is shown as a blue solid curve, with the
kerrbb contribution shown by the green dot-dashed curve, and
the cutoffpl model component shown by a red dashed curve.
The lower panel of the upper left plot shows the ratio between the
best fitting model and the data, and highlights the clear structured
residuals between the model and the data. The fit is formally
extremely poor, with a reduced chi-squared of χ2
r = 1173.12/358.
This is precisely in keeping with the finding of Fabian et al. (2020).
In the upper right panel, we show that with the addition of a hot
and small blackbody (modelled in XSPEC with the bbody model),
the structured residuals are removed from the fit, and a formally
excellent fit is found χ2
r = 353.1/356. Of course, bbody is simply a
phenomenological addition, characterized by a temperature Tbb and
radius Rbb, and has no physical content.
In contrast, in the central panel of Fig. 12 we display a joint
fit of fullkerr + cutoffpl, where fullkerr is our new
continuum fitting model which includes the intra-ISCO emission
(described in Appendices A and B). As we are now interested in the
physical parameters of the fit (in contrast to the kerrbb fit), we
fix various parameters to those with prior constraints. The source-
observer distance is fixed to D = 3 kpc (Fabian et al. 2020; Tetarenko,
5None of the models considered in this section required the addition of
a component to describe absorption of photons by neutral hydrogen (e.g.
tbabs). This is due to the relatively high starting point of the NuSTAR
bandpass (∼3 keV) and the low galactic hydrogen column density in the
direction of MAXI J1820.
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Figure 12. The Nu29 X-ray spectrum of MAXI J1820 (black points), compared to various accretion models for the emission. For each plot, we use the model
cutoffpl to model the high-energy power-law tail. In the upper left plot, we display the best-fitting kerrbb model (which employs a vanishing ISCO stress
boundary condition), which provides an extremely poor fit to the data. Adding an ad hoc single temperature blackbody component to kerrbb produces a
formally excellent fit (upper right panel). However, using a full model for the disc (one which includes intra-ISCO emission) removes the requirement for the
addition of ad hoc components. This is displayed in the central panel, where we show the excellent fit of fullkerr to the MAXI J1820 data.
Shaw Charles 2023), the black hole mass is fixed to that inferred
from optical spectroscopy M• = 8.5M (Torres et al. 2019; Tetarenko
et al. 2023), the black hole spin and source-observer inclination
are fixed to values inferred from an analysis of the hard-state X-
ray spectrum, namely a• = 0.2, i = 35◦
(Buisson et al. 2019, see
also the recent work of Dias et al. 2024). We also fix the colour-
correction factor in the main body of the disc and at the ISCO to
fd = fI = 1.7, a canonical value for X-ray binary studies (e.g. Li
et al. 2005; Davis et al. 2006). This leaves three fitting parameters,
the mass accretion rate Ṁ, the ISCO stress δJ , and the photon
starvation parameter ξ. The best-fitting values of these parameters are
Ṁ = [0.86 ± 0.02]Ledd/c2
, δJ = [3.85 ± 0.14] × 10−2
, and ξ =
1.7 ± 0.06, where the uncertainties correspond to 90 per cent
confidence intervals. This accretion rate corresponds to an Eddington
luminosity ratio of order l ≡ Ldisc/Ledd ∼ 0.1, as expected for a
soft state spectrum. The cutoffpl parameters were fit to the high
energy tail, with resulting parameter values = 1.54, Ecut = 24.7 keV,
N = 0.036 (N is a flux normalization at 1 keV). These parameters
were not allowed to vary after an initial fit to the high energy excess.
The ISCO stress parameter δJ ∼ 0.04 lies in the range typically seen
in GRMHD simulations (e.g. Noble et al. 2010; Penna et al. 2010;
Schnittman et al. 2016), and is broadly consistent with the Paczyński
(2000) estimate δJ ∼ α(H/r).
We see that the addition of intra-ISCO emission removes the
requirement for additional ad hoc thermal components, and the fit is
formally excellent χ2
r = 352.34/360. When contrasted with a fit to
kerrbb alone, the addition of intra-ISCO emission reduces the χ2
parameter by over 800, and is required at extremely high statistical
significance. We believe that this represents the first robust detection
of intra-ISCO emission in the literature.
The fact that the thermal excess at around E = 6−10 keV is sourced
from within the ISCO is shown in Fig. 13, where we explicitly split
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Figure 13. The physical origin of the different emission fit to MAXI J1820. We split the disc emission (blue solid curve) into components sourced outside
(green dot–dashed) and inside (orange dashed) the ISCO. The intra-ISCO emission provides the hot-and-small thermal component previously added ad-hoc to
vanishing ISCO stress accretion models (e.g. the upper right panel of Fig. 12).
Figure 14. The relative contributions to the total flux of the disc (blue
solid), power-law (red dashed), and extra-ISCO (green dot–dashed) and intra-
ISCO (orange dashed) emission components. The intra-ISCO emission is the
dominant source of flux for the photon energy range E ∼ 6−10 keV.
out the contributions to the total fullkerr flux (blue solid curve)
from radii outside of the ISCO (green dot dashed curve), and within
the ISCO (orange dotted curve). Contrasting Fig. 13 with the upper
right panel of Fig. 12 we see that the intra-ISCO emission is providing
precisely the additional emission modelled out by bbody in the work
of Fabian et al. (2020).
In Fig. 14, we display the fractional contributions of each of the
different emission regions to the total model flux fit to MAXI J1820.
We see that the intra-ISCO emission dominates the total emitted flux
for a relatively broad (E ∼ 6−10 keV) range of observed energies.
While the total fraction of the 0.05−50 keV disc luminosity sourced
from within the ISCO is only 4.1 per cent for this epoch, its
observational effect is pronounced in the ‘right’ energy bands. What
constitutes the right energy band is somewhat dependent on the free
parameters of the model (e.g. Fig. 8), but is typically several times the
peak temperature of the main body of the disc and therefore roughly
E ∼ 6−10 keV for typical X-ray binary parameters.
Finally, we note that the fact that observational requirement of
an observable intra-ISCO region can be leveraged to place strong
constraints on the uppermost value the black hole spin in MAXI
J1820 can take. For too large a spin, the size of the ISCO-to-event
horizon region shrinks, and the hot-and-small thermal component
becomes unobservable (e.g. Fig. 11). In Fig. 15, we refit the MAXI
J1820 X-ray spectrum for spin parameters covering the prograde
range 0 a• 0.99, and display the change in χ2
statistic as a
function of spin (upper) and ISCO-to-event horizon radial distance
(lower). In these fits the inclination i, accretion rate Ṁ, ISCO stress
δJ and photon starvation parameter ξ were allowed to vary freely.
The quality of fit is relatively insensitive to spin for low spins a• ࣠
0.4, but rapidly becomes extremely poor for spins a• 0.5. Using
these results we are able to place constraints on the MAXI J1820
black hole spin, which must be below a• ≤ 0.52 at 99.9 per cent
confidence level (Fig. 15). This result is in good agreement with the
hard state reflection modelling of Buisson et al. (2019) and Dias et al.
(2024), although disagrees with the results of Draghis et al. (2023)
(showing of course that these hard state models are inconsistent
with each other). It is unclear why Draghis et al. (2023) find such a
high spin for MAXI J1820 (a• = 0.988+0.006
−0.028), in tension with other
analyses which use the same models and data, but it may be related
to the accretion disc density they assumed, which was lower than that
expected in X-ray binary discs ne ∼ 1020
cm−3
. These higher values
of the density were used in Dias et al. (2024), who favour lower (and
even negative) spins.
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Figure 15. The change in χ2 fit statistic as a function of assumed black
hole spin (upper), or ISCO-to-event horizon distance (lower). If the spin of
MAXI J1820 is too high, there is insufficient disc area to power the required
hot-and-small thermal component, and the fit rapidly becomes very poor. The
two zoomed-in insets display the region of parameter space acceptable at a
99.9 per cent confidence level. We can constrain the black hole spin in MAXI
J1820 to be low a• 0.5, in accordance with reflection modelling in the hard
state.
MAXI J1820 was observed by Fabian et al. (2020) to require an ad-
ditional ad hoc blackbody emission component in additional epochs
to just Nu29 considered in this section. In Appendix C, we show
that, with the same fixed black hole, source-observer, and colour-
correction parameters as in this section, the epochs Nu 25, Nu27,
and Nu31 can also be described by the fullkerr + cutoffpl
model. Each epoch had a similar ISCO stress parameter δJ 0.04,
and the different epochs are principally distinguished by different
accretion rates Ṁ. Each fullkerr + cutoffpl fit represents
a similar improvement over kerrbb + cutoffpl as the Nu29
epoch discussed in this section, with fit statistic improvements of
order |χ2
| ∼ 600−800.
7 DISCUSSION
In the previous section, we focused on NuSTAR observations of
the black hole X-ray binary MAXI J1820 during a bright soft-state
outburst. In this section we discuss MAXI J1820 in the context of
the broader X-ray binary population, and include other data sets (in
particular a NICER observation of MAXI J1820) in our analysis.
Figure 16. Upper: A joint fit to simultaneous NICER (black) and NuSTAR
(purple) data of MAXI J1820, with the model components denoted by
different line styles (see legend). In the lower panel, we show the ratio of
the data to the total model for each observatory. The joint fit is statistically
acceptable. The NICER data has been corrected by a factor 1/constant with
constant 0.43 (see the text) to account for the fact that over half of the
mirror modules of NICER were switched off during this observation.
During it’s 2018 outburst, MAXI J1820 was also observed by
the NICER telescope, roughly simultaneously with the observation
presented in Section 6. NICER probes a lower energy range to
NuSTAR (NICER observes at photon energies 1−10 keV), and so
contains more information on the peak of the disc spectrum than
the NuSTAR observations. While the key signature of intra-ISCO
emission is located at photon energies E ∼ 6−10 keV, data at energies
substantially above E = 10 keV is crucial to revealing it’s presence, as
a proper handle on the properties of the comptonized power-law tail
is required so that the intra-ISCO feature is not simply modelled out
with a power-law. For this reason, we have focused on NuSTAR data,
which gives us this proper handle, but it is an interesting exercise to
see how the fullkerr model copes with the lower energy interval
probed by NICER.
In Fig. 16, we plot a joint fit to the NICER (black points) and
NuSTAR (purple points) observations of MAXI J1820. Including
this NICER data adds a couple of additional complications which
we now discuss. First, as MAXI J1820 was so bright during it’s
outburst, over half of the mirror modules of NICER were switched
off during this observation. (This was done simply to deal with the
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unusually high photon count rate of the source.) We therefore include
a multiplicative amplitude in our modelling (the model constant
in XSPEC notation) to our fitting function, which is fixed to unity for
the NuSTAR data but is best fit by constant 0.43 for the NICER
data. In addition, the lower bandpass of NICER probes an energy
range where the effects of the absorption of X-ray photons by neutral
hydrogen between the source and observer become more significant.
To model this more properly, we include the tbabs model in XSPEC
(Wilms, Allen McCray 2000). In full therefore our model is, in
the notation of XSPEC, given by
model = constant × tbabs(fullkerr + cutoffpl). (25)
Finally, at the lower energies probed by NICER, systematic errors
in the calibration of X-ray telescopes become important. Unlike
Optical telescopes, which can use nearby featureless white dwarfs,
no standard objects exist in X-ray astronomy which can be observed
and used for calibration at the per cent level. As such, it is standard
practice to add per cent level systematic errors to the X-ray data
taken from a source, to prevent bumps in the X-ray spectrum at
around 1−3 keV from dominating the statistics of the fit (this may
be particularly relevant when over half of the mirror modules are
switched off).
Using the same set of free parameters as before (in other words,
freezing the parameters M• = 8.5 M, a• = 0.2, i = 35◦
, and D =
3 kpc), and including a systematic error of 2 per cent, we find a best
fit to the joint NICER + NuSTAR data which is consistent (in terms
of the values of the physical parameters Ṁ, δJ and ξ) with our fit to
the NuSTAR data alone, and which is statistically acceptable χ2
r =
1142.19/1050. Letting any of the free parameters a•, i, or the disc
colour-correction factor fd freely vary always provides a statistically
excellent fit (for example, a freely varying colour-correction factor
in the main body of the disc has best fitting reduced chi-squared
parameter χ2
r = 986.28/1049; this fit is shown in Fig. 16). If we
allow all three of these parameters to vary freely, we find an excellent
fit even if the systematic errors in the data collection are lower (at
the 1.5 per cent level).
A key result is that the improvement of the fullkerr fit over
the model
model = constant × tbabs(kerrbb + cutoffpl), (26)
grows with the addition of the NICER data. Allowing all parameters
in the kerrbb model (other than the source-observer distance and
the vanishing ISCO stress boundary condition) to freely vary results
in a best-fitting reduced chi-squared value of χ2
r = 2657.24/1050,
which is χ2
= 1515.05 higher than our canonical model fit.
It is also worth noting that the source MAXI J1820 potentially
has, as has been suggested in a number of works (e.g. Buisson et al.
2019; Fabian et al. 2020; Poutanen et al. 2022; Thomas et al. 2022),
a large misalignment between the binary orbital inclination and the
disc’s inclination with respect to the black hole spin axis. We do not
believe that this complication has any effect on the interpretation put
forward in this paper for two reasons. First, we have verified that
by fixing the inclination of the disc to that inferred from the binary
orbit inclination (i 70◦
) we are still able to find excellent fits to
the NuSTAR data by allowing the black hole spin a•, accretion rate
Ṁ and intra-ISCO parameters δJ and ξ to vary. Secondly, while the
accretion flow may well show some large scale warping owing to
this misalignment, it is likely that the inner disc will be aligned with
the black hole’s equatorial plane at small radii (an assumption when
solving the disc equations in the fullkerr model), owing to the
Bardeen-Peterson effect (Bardeen Petterson 1975), a theoretical
model of disc-black hole alignment with numerical support (Liska
et al. 2021).
Finally, it is worth stressing the findings of Fabian et al. (2020),
namely that the excess flux observed in the spectrum of MAXI
J1820 at E ∼ 6−10 keV cannot plausibly be modelled out with
alternative explanations. Adding additional power-law components
would require power-law indices that are implausibly steep ∼ 7−8,
additional iron line components can only reproduce the data if the
geometry of the irradiating source changes by significant factors on
short timescales, and an additional Gaussian emission component
would require an equivalent width which is too large to be plausible
(we direct the interested reader to Fabian et al. 2020, for further
discussion).
In an ideal world, a final test of this model would be the continued
detection of this excess component as the disc cools into an even
lower luminosity state. This would rule out any other effects related
to the moderate L ∼ 0.1Ledd luminosity of the source in the bright
soft state. Unfortunately, as MAXI J1820 continued to dim at epochs
later than the final epoch studied in this paper (Nu31) the power-law
component thereafter grew in amplitude (and relative importance),
and subsequently dominated the spectrum rendering such a test
impossible (see e.g. fig. 1 of Fabian et al. 2020 for the full MAXI
J1820 light curve). It is important to note however that the properties
of the power-law tail and ad hoc blackbody component added by
Fabian et al. (2020) showed no correlation in properties, despite the
power-law component varying by over a factor of 40. This suggests
they are not linked physically.
We do believe however that the components discussed in this
paper should be detectable in a wider population of sources, which
may allow further tests of this model at a range of accretion rates.
Of particular interest are sources suspected to have low spins and
large inclinations, where the effects of plunging-region emission
are expected to be maximal (Figs 10 and 11). Sources with these
characteristics are known, such as LMC X-3 and H1743-322 (see
e.g. Bambi 2018, for a review of previous spin estimates), and will
be interesting avenues for future research.
7.1 Iron K α flux from within the plunging region
While the focus of this work has been on continuum emission
sourced from within the plunging region, here we briefly discuss
the implications of a non-zero density and emission for iron K-α
studies of black hole accretion discs. One major difference between
continuum fitting and reflection spectroscopy studies is that, while the
radiative temperature of the disc remains high within the plunging
region (e.g. Fig. 1), the density of the flow does drop much more
rapidly (a result of the rapid increase in the radial velocity and the
fixed radial mass flux Ṁ = 2πrUr
ρH e.g. Mummery Balbus
2023). A key implication of this result is that the disc ionization
fraction ξFe ∝ FX/ρ grows rapidly (the parameter FX is the irradiating
X-ray flux, which typically grows with decreasing radius as a power
law, although this behaviour may change at the smallest length scales
comparable to the size of the corona), and for typical parameters
the flow quickly becomes over ionized within the ISCO. Indeed,
it has been argued that this region therefore typically contributes
minimally to the time averaged X-ray reflection spectrum (e.g.
Wilkins, Reynolds Fabian 2020).
That being said, X-ray binaries represent a particularly interesting
probe of intra-ISCO reflection spectroscopy, owing to their large
electron number densities in the main body of the disc ne ∼ 1020
cm−3
, which makes them less susceptible to over ionization (when
compared to AGN discs, for example). As can be clearly seen in
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Figure 17. The chi-squared fit statistic of the fullkerr + cutoffpl
model fit to the NuSTAR data shown in Fig. 12, as a function of black hole
spin parameter a•, with the inclination fixed to i = 35◦. This inclination was
the best fitting value found by Buisson et al. 2019 when modelling the hard
state emission of MAXI J1820. We see that the spin value inferred from our
continuum fitting analysis is consistent with that found from the hard state
analysis of Buisson et al. 2019, a• = 0.2. Red dot–dashed lines show the 1,
2, and 3σ intervals, respectively.
Figs 2 and 4, the red and blue shifting of photons emitted from
the plunging region can be extreme, and may well offer interesting
probes of the intra-ISCO region (Reynolds Begelman 1997). These
calculations are being actively pursued (e.g. Dong et al. 2023).
Finally, one particularly interesting avenue for future studies will
be in examining the concordance between reflection spectroscopy
and continuum fitting black hole spin measurements, when plunging
region emission is included. As a first demonstration of these
model tests we plot in Fig. 17 the chi-squared fit statistic of the
fullkerr + cutoffpl model fit to the NuSTAR data shown
in Fig. 12, as a function of black hole spin parameter a•, with the
inclination fixed to i = 35◦
. This inclination was the best fitting
value found by Buisson et al. (2019) when modelling the hard state
emission of MAXI J1820. We see that the spin value inferred from
our continuum fitting analysis is consistent with that found from the
hard state analysis of Buisson et al. (2019), a• = 0.2. Red dot–dashed
lines show the 1, 2, and 3σ confidence intervals, respectively (with
larger confidence intervals at higher χ2
values). See Appendix C for
this same calculation performed at different epochs.
8 CONCLUSIONS
In this paper, we have extended existing X-ray continuum fitting
models to include emission sourced from within the ISCO of Kerr
black hole discs. GRMHD simulations of black hole accretion find
such emission to be a generic feature of these systems (e.g. Noble
et al. 2010; Zhu et al. 2012; Schnittman et al. 2016; Wielgus et al.
2022), driven by magnetic stresses which couple the stable and
plunging disc regions.
The extra luminosity sourced from within the ISCO is generally
observed to take the form of a hot-and-small quasi-blackbody
component (e.g. Figs 7, 8, and 10), but can for more extreme regions
of parameter space power a power-law tail (e.g. Figs 6 and 9). This
additional emission broadens and hardens the total disc spectrum, and
should in principle be observable for a wide range of parameter space.
This is true provided that black holes are not all near-maximally
rotating, as in the maximal spin limit the event horizon-to-ISCO
region shrinks and the intra-ISCO emission becomes less important
(Fig. 11).
We have then shown that the addition of intra-ISCO emission
resolves some problems for conventional disc models. In particular,
we are able to describe the emission from MAXI J1820 during a 2018
soft-state outburst, something which is not possible with conventional
models truncated at the ISCO (Fig. 12). The intra-ISCO emission
reproduces the requirements of previously added ad hoc blackbody
profiles (Fig. 13). The dominant component of the emission between
6 and 10 keV in the MAXI J1820 spectrum results from emission
sourced from within the ISCO, highlighting the importance of this
region (Fig. 14). As far as the authors are aware this work represents
the first robust detection of intra-ISCO emission in the literature.
The detection of intra-ISCO emission allows constraints to be
placed on the MAXI J1820 black hole spin, which we have demon-
strated must be low a• ≤ 0.52 (99.9 per cent confidence level) to allow
a detectable intra-ISCO region. This result is in good accordance with
the hard state reflection modelling of Buisson et al. (2019) and Dias
et al. (2024). Modelling of intra-ISCO emission has the potential to
be a powerful diagnostic of black hole parameters in the future.
As other sources (for example, MAXI J0637-430 Lazar et al. 2021)
have also been fit with ad hoc blackbody components, it seems to us
likely that observations of intra-ISCO emission may be widespread,
but previously modelled out or neglected.
ACKNOWLEDGEMENTS
The authors would like to thank the reviewer for a detailed report
which improved the manuscript. AM gratefully acknowledges sup-
port and hospitality from the Institute for Advanced Study, where
some of this work was completed. This work was supported by
a Leverhulme Trust International Professorship grant number LIP-
202-014. For the purpose of Open Access, AM has applied a CC BY
public copyright licence to any Author Accepted Manuscript version
arising from this submission. AI acknowledges support from the
Royal Society. This research has made use of data from the NuSTAR
mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the
National Aeronautics and Space Administration. We acknowledge
the use of public data from the NICER data archive.
DATA AVAILABILITY
The XSPEC model fullkerr is available at the following GitHub
repository: https://github.com/andymummeryastro/fullkerr. At this
link the X-ray spectrum of MAXI-J1820 fit in the manuscript can
also be found.
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APPENDIX A: THE DISC MODEL
In this Appendix, we list every analytical result used in the ful-
lkerr model, so that this paper remains self-contained. More
detailed treatments of both the intra- and extra-ISCO disc regions
are presented elsewhere in the literature.
A1 Orbital motion and ISCO location
The key orbital component relevant for the study of thin accretion
flows is the angular momentum of a fluid element undergoing circular
motion, as this is an excellent approximation to the dynamical
behaviour of the fluid in the stable disc regions. For the Kerr metric
standard methods (e.g. Hobson, Efstathiou Lasenby 2006) lead to
the following circular angular momentum profile
Uφ = (GMr)1/2
(1 + a2
/r2
− 2ar1/2
g /r3/2
)
1 − 3rg/r + 2ar
1/2
g /r3/2
. (A1)
The (dimensionless) energy of a circular orbit is similarly given by
Ut /c2
= −
(1 − 2rg/r + ar1/2
g /r3/2
)
1 − 3rg/r + 2ar
1/2
g /r3/2
. (A2)
In this paper, we shall define the φ coordinate to increase in the
direction of the orbital motion of the fluid. This means that Uφ(r, a)
≥ 0 for all orbits, and retrograde motion is identified with negative
Kerr spin parameters a 0.
A thin disc will persist in its classical form wherever these
orbits are stable. The stability of circular orbits requires ∂r Uφ 0,
the relativistic analogue of the Rayleigh criterion. Evaluating this
gradient, we find
∂Uφ
∂r
=
(GM)1/2
2r1/2D
1 +
ar1/2
g
r3/2
1 −
6rg
r
−
3a2
r2
+
8ar1/2
g
r3/2
,
(A3)
where
D = 1 − 3rg/r + 2ar1/2
g /r3/2 3/2
. (A4)
Note that D is finite and positive for all radii r rI of interest (where
we denote the ISCO location by rI), so equation (A3) passes through
zero at r = rI, where the final factor vanishes, i.e.:
r2
I − 6rgrI + 8a
√
rgrI − 3a2
= 0. (A5)
The location of the ISCO as a function of Kerr spin rI(a) can be
written in closed form, and is given by Bardeen, Press Teukolsky
1972)
rI
rg
= 3 + Z2 − sgn(a•)
(3 − Z1)(3 + Z1 + 2Z2), (A6)
where
a• ≡ a/rg, (A7)
is the dimensionless spin, and we have defined
Z1 = 1 + (1 − a2
•)
1
3
(1 + a•)
1
3 + (1 − a•)
1
3
(A8)
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and
Z2 = 3a2
• + Z2
1. (A9)
Another orbital motion component of use is
Ut
(r, a) =
1 + a
rg/r3
1 − 3rg/r + 2a
rg/r3
1/2
. (A10)
A2 Extra-ISCO temperature profile
In the stable regions of the disc, the temperature profile of a thin
accretion flow fed by a constant mass flux Ṁ in the general Kerr
metric gμν
is given by (Novikov Thorne 1973; Page Thorne
1974; Balbus 2017)
σT 4
= −
1
2
√
|g|
Ut 2 d
dr
Ṁ
2π
r Uφ
Ut
dr +
FJ
2π
, (A11)
where
≡
Uφ
Ut
=
GM/r3
1 + a
rg/r3
, (A12)
g is the metric determinant, and Ṁ is the constant mass flux through
the disc, while FJ is an integration constant relating to the angular
momentum flux through the disc. The temperature of the main body
of the accretion disc is therefore found by solving the integral
I(r, a) =
Ṁ
2π
r Uφ
Ut
dr +
FJ
2π
=
Ṁc
4π
r
rg
r
r2
− 6rgr − 3a2
+ 8a
√
rgr
r2 − 3rgr + 2a
√
rgr
dr +
FJ
2π
(A13)
with x ≡
r/rg and a• = a/rg, we have
I(r, a) =
Ṁrgc
2π
r
x4
− 6x2
− 3a2
• + 8a•x
x4 − 3x2 + 2a•x
dx +
FJ
2π
, (A14)
which can be solved with standard partial fraction techniques, as was
first shown in Page Thorne (1974). The roots of the lower cubic
x3
− 3x + 2a• = 0, (A15)
denoted {xλ} are
xλ = 2 cos
1
3
cos−1
(−a•) −
2πλ
3
(A16)
with λ = 0, 1, 2. The solution is then
I(r, a) =
Ṁrgc
2π
x −
3a•
2
ln(x) +
2
λ=0
kλ ln |x − xλ|
+
FJ
2π
,
(A17)
where
kλ ≡
2xλ − a•(1 + x2
λ)
2(1 − x2
λ)
. (A18)
We now choose the physical values of our integration constants. The
mass flux Ṁ simply scales the amplitude of each parameter, while
FJ determines the ISCO boundary condition. The vanishing ISCO
stress condition enforces
−
FJ ,V
Ṁ
≡ JV =
GMrI
1 −
3a•
2xI
ln(xI )
+
1
xI
2
λ=0
kλ ln |xI − xλ|
, (A19)
and the general boundary condition we shall write as
−
FJ
Ṁ
≡ JV (1 − δJ ). (A20)
The parameter JV corresponds to the specific angular momentum
that would have to be carried by each fluid element from the ISCO
to the horizon so that there is no communication between the two
disc regions. This expression defines δJ , which is our free inner disc
stress parameter. We define our inner disc parameter in this manner
as δJ is a number that can be readily determined from GRMHD
simulations of accretion discs. Physically, δJ can be thought of as
the fraction of the specific angular momentum ‘passed back’ into the
disc from the r ≤ rI region by whatever process is generating the
stress at the ISCO.
While δJ has a clear physical interpretation, it is not immediately
clear what value it should take, or upon which other physical
parameters it should depend. As we discuss in the main body of the
text, the physical origin of δJ is ultimately expected to be angular
momentum transport driven by magnetic turbulence, and no simple
scaling arguments for its parameter dependence is currently known.
Simulations provide a rough scale of δJ , placing it in the range
of ∼0.01−0.2 (Shafee et al. 2008; Noble et al. 2010; Penna et al.
2010), but also suggest that δJ may depend on factors including the
magnetic field topology of the simulation (for example, whether the
initial field geometry comprised of 1 or 4 field loops Penna et al.
2010). Intuitively, it seems likely that δJ will depend on factors
such as the overall disc magnetization (a ‘MAD’ or ‘magnetically
arrested disc’ can in some ways be thought of as an extreme ‘stress’
sourced from magnetic field, for example). Gammie (1999) derives
a parametrization for the ISCO stress entirely in terms of a magnetic
field strength at the ISCO, but makes the assumption of a cold
(zero temperature) gas, which is not ideal for our continuum fitting
purposes.
Given the anticipated scaling of δJ with properties of the disc
magnetic field, we anticipate that otherwise similar black holes (in
terms of mass M and spin a•) may have quite different values of δJ .
We reiterate that observational studies, and in particular parameter
inference studies of δJ , may have much to teach us about this region.
Folding this result through to the key radiative temperature profile,
we find (equation A11)
σT 4
R =
3GMṀ
8πr3
1 −
3a•
2x
ln(x) +
1
x
2
λ=0
kλ ln |x − xλ|
−
JV (1 − δJ )
√
GMr
1 −
3
x2
+
2a•
x3
−1
. (A21)
This is the extra-ISCO temperature profile used in the fullkerr
model, and also serves to determine the thermodynamic boundary
condition for the post-ISCO plunge.
A3 Intra-ISCO disc
Unlike the extra-ISCO disc regions, inside the ISCO the evolution
of the disc temperature depends on all thermodynamic quantities,
not just the local mass flux Ṁ and angular momentum flux FJ .
Assuming an ideal fluid stress energy tensor
T μν
=
ρ +
P + e
c2
Uμ
Uν
+ Pgμν
+ T μν
EM, (A22)
where P, e, and ρ correspond to the total pressure, energy density
and (rest) mass density of the fluid, respectively, and T μν
EM is the
electromagnetic stress-energy tensor, which does not enter the energy
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18. Continuum emission from within the ISCO 383
MNRAS 531, 366–386 (2024)
equation in the ideal MHD limit (Mummery Balbus 2023). The
energy equation of the fluid can be expressed
Uν∇μT μν
= 0, (A23)
or explicitly
de
dr
−
P + e
ρ
dρ
dr
= 0. (A24)
This is the fundamental thermodynamic equation within the ISCO
which we solve. We must supplement this equation with the following
expressions valid inside of the ISCO
c2
s ≡
P
ρ
, (A25)
H = cs
r4
2GM•rI
, (A26)
ρ ≡
H
, (A27)
P = Pg + Pr ≡
ρkTc
μmp
+
4σT 4
c
3c
, (A28)
T 4
c =
3κ
8
T 4
R , (A29)
=
Ṁ
2πr|Ur |
, (A30)
e =
3
2
Pg + 3Pr , (A31)
Ur
= −c
2rg
3rI
rI
r
− 1
3/2
− α1/2
cs,I . (A32)
These are, in order, the definition of the speed of sound, the solution
of vertical hydrostatic equilibrium, the definition of the disc density
and pressure, the approximate solution of radiative transfer in the disc
atmosphere, the conservation of mass in the disc, the definition of
the energy density and the geodesic plunge solution with trans-ISCO
velocity given by the typical velocity fluctuation scale.
Equations (A25)–(A32) are sufficient to close equation (A24),
which becomes a first order ordinary differential equation for Tc(r).
We solve this equation numerically in fullkerr. Equation (A29)
then gives the radiative temperature used in the disc model (cf. Fig. 1).
In certain limits, the radiative temperature can be written as an
analytical function of radius, an analysis of which was performed
in Mummery Balbus (2023). If radiation pressure dominates over
gas pressure then (Mummery Balbus 2023)
TR = TR,I
rI
r
17/28
ε−1
rI
r
− 1
3/2
+ 1
−1/28
, (A33)
while if gas pressure dominates then (Mummery Balbus 2023)
TR = TR,I
rI
r
5/4
ε−1
rI
r
− 1
3/2
+ 1
−1/4
. (A34)
In these expressions anything with a subscript I is evaluated at the
ISCO, and
ε ≡
α1/2
cs,I
c
3rI
2rg
1. (A35)
In both of these expressions, we have assumed that electron scattering
opacity dominates over the free–free opacity.
In addition to the radiative temperature, all thermodynamic quan-
tities of the disc can be solved for within the ISCO by suitable
manipulation of equations (A24)–(A32). Of relevance for the physics
of photon starvation (Section 4) is the vertical structure of the disc,
as the scale height sets both the photon diffusion time-scale and
ultimately the number of photons which can be produced by free-
free processes across the disc thickness. For an arbitrary adiabatic
equation of state e = P/( − 1), the disc scale height can be solved
for exactly (Mummery Balbus 2023), and is given by
H
HI
1+
=
rI
r
−5
ε−1
rI
r
− 1
3/2
+ 1
1−
. (A36)
An important, and potentially counter-intuitive, result of the above
theory is that the scale height of the disc drops over the plunging
region (i.e. the disc gets thinner over the plunge).
A4 Vertical gravity
The (dimensionless) relativistic vertical gravity correction factor
(Abramowicz et al. 1997) is given by
Rz(r, a) =
U2
φ /(r2
g c2
) − a2
• U2
t /c2
− 1
r/rg
. (A37)
A result valid at all radii. Outside of the ISCO the fluid’s orbital
4-momentum elements are given by the results listed in equations
(A1) and (A2). Inside the ISCO, when Uφ and Ut are conserved
and given by their ISCO values, this result simplifies dramatically to
(Mummery Balbus 2023)
Rz(r, a) =
2rI
r
. (A38)
APPENDIX B: PARAMETERS OF THE FULLKERR
CONTINUUM FITTING XSPEC MODEL
The fullkerr continuum fitting model takes as an input the free
parameters listed in Table B1. We treat the colour-correction in the
main extra-ISCO body of the disc by a single number fd, which is in
principle a free parameter in the fits (although it was fixed to fd = 1.7
for the MAXI J1820 fits in this paper). In the XSPEC model, we also
allow for the use of the Done et al. (2012) temperature dependent
model (specified in XSPEC by fd = −1), but as the NuSTAR spectra
probed high photon energies E 3 keV, we found no sensitivity to
the exact extra-ISCO fcol parametrization for MAXI J1820.
The fullkerr model assumes a Shakura Sunyaev (1973)
α-parameter of α = 0.1. Again, the spectra are only very weakly
dependent on α, and this is hard coded for convenience. In this
model we restrict the model to purely black hole spacetimes (i.e.
|a•| ≤ 1), and do not consider naked singularity spacetimes (cf.
Table B1. The parameters of the fullkerr model, their units and allowed
ranges. The accretion rate parameter is defined in terms of the Eddington
luminosity, which equals Ledd = 1.26 × 1038(M/M) erg s−1. One sided
ranges denote physically allowed values, e.g. positive black hole masses.
Parameter Units Allowed range
M M M 0
a• −1 a• 1
i Degrees 0◦ i 90◦
Ṁ Ledd/c2 Ṁ 0
δJ δJ ≥ 0
fd fd ≥ 1
fI fI ≥ 1
ξ ξ 0
norm 1/kpc2 norm 0
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Mummery, Balbus Ingram 2024b). The reason for this is the intra-
ISCO behaviour of the disc fluid near r = 0 is observable for a naked
singularity disc, and the models developed in Mummery Balbus
(2023) break down in this region.
APPENDIX C: FITS TO OTHER EPOCHS OF
MAXI J1820
In Table C1, we list the best fitting fullkerr fitting parameters
to the other MAXI J1820 epochs. We also list the fit statistic of
this model and the improvement in the fit statistic compared to a
kerrbb + cutoffpl model. For these fits, we fix the black
hole parameters to M = 8.5M, a• = 0.2, the source-observer
parameters to i = 35◦
, D = 3 kpc, and the colour-correction
parameters to fd = fI = 1.7. Formally better fits are possible if
these parameters are allowed to freely vary, but the improvement over
kerrbb + cutoffpl is so strong that we deem this unnecessary.
The chief cause of model-data discrepancies is now at photon
energies E ≥ 10 keV, where the spectrum is dominated by power-law
emission and not the disc.
The fitted parameters are in the same units as discussed in the
main body of the text (see also Table B1). See Fabian et al. (2020)
for more details of the individual epochs. Parameter confidence
intervals are 90 per cent intervals. The luminosity Eddington ratio
Table C1. Best-fitting parameters of the fullkerr model to each MAXI
J1820 epoch, the fit statistic of this model and the improvement in the fit
statistic compared to a kerrbb + cutoffpl model. Parameters are in the
same units as discussed in the main body of the text. See Fabian et al. (2020)
for more details of the individual epochs. Parameter confidence intervals are
90 per cent intervals. The luminosity Eddington ratio is roughly 10 per cent
of the accretion rate parameter for the chosen black hole spin.
Epoch Ṁ δJ ξ χ2
r,f k χ2
f k−kbb
Nu25 1.15+0.02
−0.02 0.043+0.001
−0.001 1.91+0.05
−0.05
888.8
858 −629.8
Nu27 1.05+0.01
−0.01 0.040+0.001
−0.001 1.49+0.04
−0.04
982.1
858 −785.4
Nu29 0.86+0.02
−0.02 0.039+0.002
−0.002 1.70+0.06
−0.06
352.3
360 −820.7
Nu31 0.79+0.01
−0.01 0.036+0.001
−0.001 1.85+0.03
−0.03
518.6
461 −816.0
Figure C1. Spin constraints at fixed inclination (i = 35◦) for each of
the different epochs of MAXI J1820 data. Horizontal dot–dashed curves
correspond to 1, 2, and 3σ constraints (in order of increasing χ2). Epoch
25 is inconsistent with the other epochs at ∼2σ, but this is likely the result of
the more prominent (and complex) power-law component in this epoch.
Figure C2. Similar fits to Figs 12–14 but for epoch Nu25 (see Fabian et al.
2020, for more details). See the text for fixed and fitted parameter values.
is roughly 10 per cent of the accretion rate parameter for the chosen
black hole spin, and varies by roughly 50 per cent over the four
observations. The fraction of the total 0.05−50 keV luminosity
sourced from within the ISCO for the four epochs listed was
4.5 per cent, 4.3 per cent, 4.1 per cent and 3.8 per cent, respectively.
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