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.
Betelgeuse as a Merger of a Massive Star with a CompanionSérgio Sacani
This document summarizes a study that uses 3D hydrodynamic simulations and 1D stellar evolution modeling to investigate the merger of a 16 solar mass star with a 4 solar mass companion star. The simulations show the companion spirals inward and merges with the primary star's helium core. Approximately 0.6 solar masses of material is ejected in an asymmetric, bipolar outflow. The post-merger structure is then modeled in 1D stellar evolution, showing in some cases the star evolves to have surface properties similar to Betelgeus, with rapid rotation and enhanced nitrogen at the surface. This pioneering study aims to comprehensively model stellar mergers across dynamical, thermal, and nuclear evolutionary timescales.
Hot Earth or Young Venus? A nearby transiting rocky planet mysterySérgio Sacani
Venus and Earth provide astonishingly different views of the evolution of a rocky planet, raising the question of why these two rock y worlds evolv ed so differently. The recently disco v ered transiting Super-Earth LP 890-9c (TOI-4306c, SPECULOOS-2c) is a key to the question. It circles a nearby M6V star in 8.46 d. LP890-9c receives similar flux as modern Earth, which puts it very close to the inner edge of the Habitable Zone (HZ), where models differ strongly in their prediction of how long rocky planets can hold onto their water. We model the atmosphere of a hot LP890-9c at the inner edge of the HZ, where the planet could sustain several very different environments. The resulting transmission spectra differ considerably between a hot, wet exo-Earth, a steamy planet caught in a runaway greenhouse, and an exo-Venus. Distinguishing these scenarios from the planet’s spectra will provide critical new insights into the evolution of hot terrestrial planets into exo-Venus. Our model and spectra are available online as a tool to plan observations. They show that observing LP890-9c can provide key insights into the evolution of a rocky planet at the inner edge of the HZ as well as the long-term future of Earth.
Fizzy Super-Earths: Impacts of Magma Composition on the Bulk Density and Stru...Sérgio Sacani
Lava worlds are a potential emerging population of Super-Earths that are on close-in orbits around their host stars,
with likely partially molten mantles. To date, few studies have addressed the impact of magma on the observed
properties of a planet. At ambient conditions, magma is less dense than solid rock; however, it is also more
compressible with increasing pressure. Therefore, it is unclear how large-scale magma oceans affect planet
observables, such as bulk density. We update ExoPlex, a thermodynamically self-consistent planet interior
software, to include anhydrous, hydrous (2.2 wt% H2O), and carbonated magmas (5.2 wt% CO2). We find that
Earth-like planets with magma oceans larger than ∼1.5 R⊕ and ∼3.2 M⊕ are modestly denser than an equivalentmass
solid planet. From our model, three classes of mantle structures emerge for magma ocean planets: (1) a
mantle magma ocean, (2) a surface magma ocean, and (3) one consisting of a surface magma ocean, a solid rock
layer, and a basal magma ocean. The class of planets in which a basal magma ocean is present may sequester
dissolved volatiles on billion-year timescales, in which a 4 M⊕ mass planet can trap more than 130 times the mass
of water than in Earth’s present-day oceans and 1000 times the carbon in the Earth’s surface and crust.
This document discusses evidence that the Moon-forming impact occurred later than previously thought, at around 95 million years after the formation of the solar system. The study uses simulations of planetary formation to show a correlation between the timing of the last giant impact and the amount of mass later accreted by the planet. Comparing this to highly siderophile element abundances in Earth's mantle, which constrain the amount of late-accreted mass, the study determines the Moon-forming impact was most likely 95 million years after solar system formation. Earlier times of 40 million years or less are ruled out at a 99.9% confidence level. The simulations include both classical scenarios and scenarios where Jupiter and Saturn migrated inward early in the solar
Disks of Stars in the Galactic Center Triggered by Tidal Disruption EventsSérgio Sacani
This document proposes that tidal disruption events (TDEs) from wandering stars could trigger episodes of positive star formation feedback in the Galactic Center, providing an explanation for the observed disks of young stars near Sgr A*. When a star is tidally disrupted by the supermassive black hole, the resulting jet compresses gas clouds to densities high enough to resist tidal forces and form stars within the disk plane perpendicular to the jet. The estimated rate of jetted TDEs is consistent with the age of the disk stars. This mechanism predicts a random orientation for each disk and the potential for multiple misaligned disks from separate TDE events.
The SAMI Galaxy Sur v ey: galaxy spin is more strongly correlated with stella...Sérgio Sacani
We use the SAMI Galaxy Surv e y to examine the drivers of galaxy spin, λR e , in a multidimensional parameter space including stellar mass, stellar population age (or specific star formation rate), and various environmental metrics (local density, halo mass, satellite versus central). Using a partial correlation analysis, we consistently find that age or specific star formation rate is the primary parameter correlating with spin. Light-weighted age and specific star formation rate are more strongly correlated with spin than mass-weighted age. In fact, across our sample, once the relation between light-weighted age and spin is accounted for, there is no significant residual correlation between spin and mass, or spin and environment. This result is strongly suggestive that the present-day environment only indirectly influences spin, via the removal of gas and star formation quenching. That is, environment affects age, then age affects spin. Older galaxies then have lower spin, either due to stars being born dynamically hotter at high redshift, or due to secular heating. Our results appear to rule out environmentally dependent dynamical heating (e.g. g alaxy–g alaxy interactions) being important, at least within 1 R e where our kinematic measurements are made. The picture is more complex when we only consider high-mass galaxies ( M ∗ ≳ 10 11 M ). While the age-spin relation is still strong for these high-mass galaxies, there is a residual environmental trend with central galaxies preferentially having lower spin, compared to satellites of the same age and mass. We argue that this trend is likely due to central galaxies being a preferred location for mergers.
Venus and Earth have remarkably diferent
surface conditions, yet the lithospheric
thickness and heat fow on Venus may be
Earth-like. This fnding supports a tectonic
regime with limited surface mobility and
dominated by intrusive magmatism.
The document discusses nucleosynthesis in the early universe and provides evidence for the Big Bang theory. It explains that during the first three minutes after the Big Bang, most deuterium combined to form helium and trace amounts of lithium. The predicted abundances of these light elements depend on the density of ordinary matter and agree well with observations, providing strong evidence for the Big Bang.
Betelgeuse as a Merger of a Massive Star with a CompanionSérgio Sacani
This document summarizes a study that uses 3D hydrodynamic simulations and 1D stellar evolution modeling to investigate the merger of a 16 solar mass star with a 4 solar mass companion star. The simulations show the companion spirals inward and merges with the primary star's helium core. Approximately 0.6 solar masses of material is ejected in an asymmetric, bipolar outflow. The post-merger structure is then modeled in 1D stellar evolution, showing in some cases the star evolves to have surface properties similar to Betelgeus, with rapid rotation and enhanced nitrogen at the surface. This pioneering study aims to comprehensively model stellar mergers across dynamical, thermal, and nuclear evolutionary timescales.
Hot Earth or Young Venus? A nearby transiting rocky planet mysterySérgio Sacani
Venus and Earth provide astonishingly different views of the evolution of a rocky planet, raising the question of why these two rock y worlds evolv ed so differently. The recently disco v ered transiting Super-Earth LP 890-9c (TOI-4306c, SPECULOOS-2c) is a key to the question. It circles a nearby M6V star in 8.46 d. LP890-9c receives similar flux as modern Earth, which puts it very close to the inner edge of the Habitable Zone (HZ), where models differ strongly in their prediction of how long rocky planets can hold onto their water. We model the atmosphere of a hot LP890-9c at the inner edge of the HZ, where the planet could sustain several very different environments. The resulting transmission spectra differ considerably between a hot, wet exo-Earth, a steamy planet caught in a runaway greenhouse, and an exo-Venus. Distinguishing these scenarios from the planet’s spectra will provide critical new insights into the evolution of hot terrestrial planets into exo-Venus. Our model and spectra are available online as a tool to plan observations. They show that observing LP890-9c can provide key insights into the evolution of a rocky planet at the inner edge of the HZ as well as the long-term future of Earth.
Fizzy Super-Earths: Impacts of Magma Composition on the Bulk Density and Stru...Sérgio Sacani
Lava worlds are a potential emerging population of Super-Earths that are on close-in orbits around their host stars,
with likely partially molten mantles. To date, few studies have addressed the impact of magma on the observed
properties of a planet. At ambient conditions, magma is less dense than solid rock; however, it is also more
compressible with increasing pressure. Therefore, it is unclear how large-scale magma oceans affect planet
observables, such as bulk density. We update ExoPlex, a thermodynamically self-consistent planet interior
software, to include anhydrous, hydrous (2.2 wt% H2O), and carbonated magmas (5.2 wt% CO2). We find that
Earth-like planets with magma oceans larger than ∼1.5 R⊕ and ∼3.2 M⊕ are modestly denser than an equivalentmass
solid planet. From our model, three classes of mantle structures emerge for magma ocean planets: (1) a
mantle magma ocean, (2) a surface magma ocean, and (3) one consisting of a surface magma ocean, a solid rock
layer, and a basal magma ocean. The class of planets in which a basal magma ocean is present may sequester
dissolved volatiles on billion-year timescales, in which a 4 M⊕ mass planet can trap more than 130 times the mass
of water than in Earth’s present-day oceans and 1000 times the carbon in the Earth’s surface and crust.
This document discusses evidence that the Moon-forming impact occurred later than previously thought, at around 95 million years after the formation of the solar system. The study uses simulations of planetary formation to show a correlation between the timing of the last giant impact and the amount of mass later accreted by the planet. Comparing this to highly siderophile element abundances in Earth's mantle, which constrain the amount of late-accreted mass, the study determines the Moon-forming impact was most likely 95 million years after solar system formation. Earlier times of 40 million years or less are ruled out at a 99.9% confidence level. The simulations include both classical scenarios and scenarios where Jupiter and Saturn migrated inward early in the solar
Disks of Stars in the Galactic Center Triggered by Tidal Disruption EventsSérgio Sacani
This document proposes that tidal disruption events (TDEs) from wandering stars could trigger episodes of positive star formation feedback in the Galactic Center, providing an explanation for the observed disks of young stars near Sgr A*. When a star is tidally disrupted by the supermassive black hole, the resulting jet compresses gas clouds to densities high enough to resist tidal forces and form stars within the disk plane perpendicular to the jet. The estimated rate of jetted TDEs is consistent with the age of the disk stars. This mechanism predicts a random orientation for each disk and the potential for multiple misaligned disks from separate TDE events.
The SAMI Galaxy Sur v ey: galaxy spin is more strongly correlated with stella...Sérgio Sacani
We use the SAMI Galaxy Surv e y to examine the drivers of galaxy spin, λR e , in a multidimensional parameter space including stellar mass, stellar population age (or specific star formation rate), and various environmental metrics (local density, halo mass, satellite versus central). Using a partial correlation analysis, we consistently find that age or specific star formation rate is the primary parameter correlating with spin. Light-weighted age and specific star formation rate are more strongly correlated with spin than mass-weighted age. In fact, across our sample, once the relation between light-weighted age and spin is accounted for, there is no significant residual correlation between spin and mass, or spin and environment. This result is strongly suggestive that the present-day environment only indirectly influences spin, via the removal of gas and star formation quenching. That is, environment affects age, then age affects spin. Older galaxies then have lower spin, either due to stars being born dynamically hotter at high redshift, or due to secular heating. Our results appear to rule out environmentally dependent dynamical heating (e.g. g alaxy–g alaxy interactions) being important, at least within 1 R e where our kinematic measurements are made. The picture is more complex when we only consider high-mass galaxies ( M ∗ ≳ 10 11 M ). While the age-spin relation is still strong for these high-mass galaxies, there is a residual environmental trend with central galaxies preferentially having lower spin, compared to satellites of the same age and mass. We argue that this trend is likely due to central galaxies being a preferred location for mergers.
Venus and Earth have remarkably diferent
surface conditions, yet the lithospheric
thickness and heat fow on Venus may be
Earth-like. This fnding supports a tectonic
regime with limited surface mobility and
dominated by intrusive magmatism.
The document discusses nucleosynthesis in the early universe and provides evidence for the Big Bang theory. It explains that during the first three minutes after the Big Bang, most deuterium combined to form helium and trace amounts of lithium. The predicted abundances of these light elements depend on the density of ordinary matter and agree well with observations, providing strong evidence for the Big Bang.
Large-scale Volcanism and the Heat Death of Terrestrial WorldsSérgio Sacani
This document discusses the potential for large igneous provinces (LIPs) to cause the "heat death" of terrestrial planets through massive volcanic eruptions that overwhelm the climate system. It examines the timing of LIP events on Earth to estimate the likelihood of nearly simultaneous eruptions. Statistical analysis of Earth's LIP record finds that eruptions within 0.1-1 million years of each other are likely. Simultaneous LIPs could have driven Venus into a runaway greenhouse effect like its current state. The timing of LIP events on Earth provides insight into potential past LIP activity on Venus that may have ended its hypothesized earlier temperate climate.
Periodic mass extinctions_and_the_planet_x_model_reconsideredSérgio Sacani
The 27 Myr periodicity in the fossil extinction record has been con-
firmed in modern data bases dating back 500 Myr, which is twice the time
interval of the original analysis from thirty years ago. The surprising regularity
of this period has been used to reject the Nemesis model. A second
model based on the sun’s vertical galactic oscillations has been challenged
on the basis of an inconsistency in period and phasing. The third astronomical
model originally proposed to explain the periodicity is the Planet
X model in which the period is associated with the perihelion precession
of the inclined orbit of a trans-Neptunian planet. Recently, and unrelated
to mass extinctions, a trans-Neptunian super-Earth planet has been proposed
to explain the observation that the inner Oort cloud objects Sedna
and 2012VP113 have perihelia that lie near the ecliptic plane. In this
Letter we reconsider the Planet X model in light of the confluence of the
modern palaeontological and outer solar system dynamical evidence.
Key Words: astrobiology - planets and satellites - Kuiper belt:
general - comets: general
The document describes simulations of a collision between the Moon and a companion moon approximately 1/3 the diameter of the Moon. The simulations found that at the modeled subsonic impact velocity, the companion moon did not form an impact crater but was instead accreted onto the Moon's surface. This added material contributed a hemispheric layer comparable to the extent and thickness of the lunar farside highlands. The collision also displaced the Moon's magma ocean to the opposite hemisphere, potentially explaining the observed concentration of KREEP materials. The findings suggest this late accretion event could explain the geological dichotomy between the lunar near and farside regions.
Theory of Planetary System Formation The mass of the presol.pdfadislifestyle
Theory of Planetary System Formation The mass of the pre-solar molecular cloud played the
largest role in terms of how the solar system formed. It might have begun with a 100 solar mass
cloud approximately 1 to 2 light years in diameter. It's possible that mutual gravitational attraction
between cloud particles was too weak to start the process. When gravity is too weak, the only
other force strong enough to bring a significant number of particles together is the electromagnetic
force. Barring that, perhaps a nearby shockwave from a supernova explosion caused the initial
motion of material: but once started, gravity took hold, causing the inevitable collapse. The
process it underwent followed a pattern that scientists believe is mirrored everywhere a star exists.
In this activity, you will put the solar system formation process parts in order from the beginning. 1.
Planetesimals accreted material until they became large enough to form planets. 2. Gravitational
potential energy of the collapsing gas cloud was converted into thermal energy. 3. Collapsing gas
cloud rotated faster as the collapse continued due to conservation of angular momentum. 4.
Planetesimals were massive enough to have a gravitational field sufficient to attract additional
nearby objects. 5. The random motions of material in the collapsing gas cloud were reduced to the
final motion of the material rotating in a disk. 6. The inner parts of the continuing, flattening cloud
free fell into the growing object at the center. 7. Continued motions brushed smaller particle grains
against larger grains. As this electrostatic "sticking" occurred, the particle grains became larger. 8.
Cloud of molecular gas started to collapse due to gravity or other astrophysical process. Use the
number of the process to order them from earliest to latest (left to right).Temperature and
Formation of Our Solar System Temperature was the key factor leading to the state distribution of
various objects made of different elements and compounds. The graph below shows the
temperature (expressed in kelvins) at different distances from the Sun (expressed in AU ) in the
solar system during the time when the planets were formed. To produce a linear plot, in the usual
sense, the vertical axis is inverted so that temperature goes from high to low starting near the Sun.
Use Figure 1 to fill in Table 1 with the formation temperatures for each planet, including the dwarf
planet, Ceres.Aktranomy 1511 Laboratory Manua! Bond albedo refers to the total radiation
reflected from an object compared to the total incident radiation from the Sun. The geometric
albedo refers to the amount of radiation equally reflected in all directions at all wavelengths off an
object. It is clear that a wide range of planetary formation temperatures existed in the early solar
system. The temperatures at which different compounds form or for which elements have physical
state changes will vary. Since the majority of material in the molecular cl.
Jack Oughton - Galaxy Formation Journal 02.docJack Oughton
1) The document discusses theories of galaxy formation from the early universe following the Big Bang.
2) It describes the top-down and bottom-up theories of galaxy formation, where top-down suggests the first objects to form were large irregular structures that later broke apart, and bottom-up suggests smaller dense areas first combined together to form galaxies.
3) The author argues the bottom-up theory of smaller areas hierarchically clustering together is most credible given current evidence of hierarchical clustering in the universe, but knowledge in this area remains limited.
This document provides an overview of the atmospheres of the Jovian planets (Jupiter, Saturn, Uranus, and Neptune). It discusses the composition and structure of their atmospheres based on equilibrium cloud condensation models. The atmospheres contain temperature minima at the tropopause, above which temperatures increase due to absorption of sunlight, and below which temperatures increase with depth due to convection. While early models predicted ammonia and water cloud decks, spacecraft observations have since directly observed ammonia clouds on Jupiter but found they are short-lived, suggesting other cloud composition processes.
Constraints on Ceres’ internal structure and evolution from its shape and gra...Sérgio Sacani
Ceres is the largest body in the asteroid belt with a radius of
approximately 470 km. In part due to its large mass, Ceres more closely approaches
hydrostatic equilibrium than major asteroids. Pre-Dawn mission
shape observations of Ceres revealed a shape consistent with a hydrostatic
ellipsoid of revolution. The Dawn spacecraft Framing Camera has been imaging
Ceres since March 2015, which has led to high-resolution shape models
of the dwarf planet, while the gravity field has been globally determined to
a spherical harmonic degree 14 (equivalent to a spatial wavelength of 211 km)
and locally to 18 (a wavelength of 164 km). We use these shape and gravity
models to constrain Ceres’ internal structure. We find a negative correlation
and admittance between topography and gravity at degree 2 and order
2. Low admittances between spherical harmonic degrees 3 and 16 are well
explained by Airy isostatic compensation mechanism. Different models of isostasy
give crustal densities between 1200 and 1400 kg=m3 with our preferred model
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.
The SPHERE view of three interacting twin disc systems in polarised lightSérgio Sacani
Dense stellar environments as hosts of ongoing star formation increase the probability of gravitational encounters among stellar
systems during the early stages of evolution. Stellar interaction may occur through non-recurring, hyperbolic or parabolic passages
(a so-called ‘fly-by’), through secular binary evolution, or through binary capture. In all three scenarios, the strong gravitational
perturbation is expected to manifest itself in the disc structures around the individual stars. Here, we present near-infrared
polarised light observations that were taken with the SPHERE/IRDIS instrument of three known interacting twin-disc systems:
AS 205, EM* SR 24, and FU Orionis. The scattered light exposes spirals likely caused by the gravitational interaction. On
a larger scale, we observe connecting filaments between the stars. We analyse their very complex polarised intensity and put
particular attention to the presence of multiple light sources in these systems. The local angle of linear polarisation indicates
the source whose light dominates the scattering process from the bridging region between the two stars. Further, we show
that the polarised intensity from scattering with multiple relevant light sources results from an incoherent summation of the
individuals’ contribution. This can produce nulls of polarised intensity in an image, as potentially observed in AS 205.We discuss
the geometry and content of the systems by comparing the polarised light observations with other data at similar resolution,
namely with ALMA continuum and gas emission. Collective observational data can constrain the systems’ geometry and stellar
trajectories, with the important potential to differentiate between dynamical scenarios of stellar interaction.
1) Global climate models that include sophisticated cloud schemes show that tidally locked planets can develop thick water clouds near the substellar point due to strong convection. These clouds greatly increase the planetary albedo and stabilize temperatures, allowing habitability at twice the stellar flux previously thought possible.
2) The cloud feedback is stabilizing, as higher stellar flux produces stronger convection and higher albedos. Substellar clouds can block outgoing radiation, reducing the day-night temperature contrast.
3) Non-tidally locked planets do not experience this stabilizing cloud feedback, as clouds only form over parts of the tropics and mid-latitudes. Their albedo decreases with increasing stellar flux, producing a destabil
A Tale of 3 Dwarf Planets: Ices and Organics on Sedna, Gonggong, and Quaoar f...Sérgio Sacani
The dwarf planets Sedna, Gonggong, and Quaoar are interesting in being somewhat smaller than
the methane-rich bodies of the Kuiper Belt (Pluto, Eris, Makemake), yet large enough to be
spherical and to have possibly undergone interior melting and differentiation. They also reside
on very different orbits, making them an ideal suite of bodies for untangling effects of size and
orbit on present day surface composition. We observed Sedna, Gonggong, and Quaoar with the
NIRSpec instrument on the James Webb Space Telescope (JWST). All three bodies were
observed in the low-resolution prism mode at wavelengths spanning 0.7 to 5.2 μm. Quaoar was
additionally observed at 10x higher spectral resolution from 0.97 to 3.16 μm using mediumresolution gratings. Sedna’s spectrum shows a large number of absorption features due to ethane
(C2H6), as well as acetylene (C2H2), ethylene (C2H4), H2O, and possibly minor CO2.
Gonggong’s spectrum also shows several, but fewer and weaker, ethane features, along with
stronger and cleaner H2O features and CO2 complexed with other molecules. Quaoar’s prism
spectrum shows even fewer and weaker ethane features, the deepest and cleanest H2O features, a
feature at 3.2 μm possibly due to HCN, and CO2 ice. The higher-resolution medium grating
spectrum of Quaoar reveals several overtone and combination bands of ethane and methane
(CH4). Spectra of all three objects show steep red spectral slopes and strong, broad absorptions
between 2.7 and 3.6 μm indicative of complex organic molecules. The suite of light
hydrocarbons and complex organic molecules are interpreted as the products of irradiation of
methane. The differences in apparent abundances of irradiation products among these three
similarly-sized bodies are likely due to their distinctive orbits, which lead to different timescales
of methane retention and to different charged particle irradiation environments. In all cases,
however, the continued presence of light hydrocarbons implies a resupply of methane to the
2
surface. We suggest that these three bodies have undergone internal melting and geochemical
evolution similar to the larger dwarf planets and distinct from all smaller KBOs. The feature
identification presented in this paper is the first step of analysis, and additional insight into the
relative abundances and mixing states of materials on these surfaces will come from future
spectral modeling of these data.
Tidal star-planet interaction and its observed impact on stellar activity in ...Sérgio Sacani
This study investigates tidal star-planet interaction by analyzing X-ray observations of planet-hosting stars that are part of wide binary systems. The study compares the X-ray luminosity, an indicator of stellar activity, between the planet-hosting primary star and its non-planet hosting companion star. By analyzing 34 such binary systems with X-ray data from XMM-Newton and Chandra, the study finds that planet hosts with close-in massive planets have higher X-ray luminosity compared to their companion stars, indicating tidal interaction is altering the rotation and magnetic activity of the host stars. The study concludes tidal interaction from massive, close-in planets can impact the rotational evolution of stars, while more distant or smaller planets likely
The Dynamical Consequences of a Super-Earth in the Solar SystemSérgio Sacani
Placing the architecture of the solar system within the broader context of planetary architectures is one of the
primary topics of interest within planetary science. Exoplanet discoveries have revealed a large range of system
architectures, many of which differ substantially from the solar system’s model. One particular feature of exoplanet
demographics is the relative prevalence of super-Earth planets, for which the solar system lacks a suitable analog,
presenting a challenge to modeling their interiors and atmospheres. Here we present the results of a large suite of
dynamical simulations that insert a hypothetical planet in the mass range 1–10 M⊕ within the semimajor axis range
2–4 au, between the orbits of Mars and Jupiter. We show that, although the system dynamics remain largely
unaffected when the additional planet is placed near 3 au, Mercury experiences substantial instability when the
additional planet lies in the range 3.1–4.0 au, and perturbations to the Martian orbit primarily result when the
additional planet lies in the range 2.0–2.7 au. We further show that, although Jupiter and Saturn experience
relatively small orbital perturbations, the angular momentum transferred to the ice giants can result in their ejection
from the system at key resonance locations of the additional planet. We discuss the implications of these results for
the architecture of the inner and outer solar system planets, and for exoplanetary systems
All astronomical bodies originate inside clouds of gas and dust, therefore there should be a common process that leads to
their condensation. In a galactic cloud there is always a gradient of speeds from point to point. Thanks to it, vortices originate
that rake the material of the surrounding cloud gradually forming large gaseous disks, inside which vortices of second order
develop that concentrate the matter of their orbits forming smaller and much denser disks, within which third order vortices
further concentrate the matter. The dense cores of these vortices finally condense in massive bodies: sun, planets and satellites.
The result should be a well ordered planetary system with no “debris” around and where both planets and satellites obey to
a precise rule of the distances from their central body. The solar system complies with these conditions with three main
exceptions. First, in an orbit where a large planet should be there is only a huge number of scattered asteroids. Second, Earth
and its moon with all evidence were not formed in the same vortex, which means that Moon originated somewhere else. Third,
Neptune’s satellite system has been shattered by the intrusion of a foreign body, Triton, and its largest satellites are missing.
These exceptions seem to be strictly connected to each other and all due to a unique event, that is: Triton has diverted the
largest Neptune satellite towards the Sun. This satellite impacted at high speed against the missing planet, scattering myriads
of fragments from its mantle and pushing it towards the sun, where it eventually fell. The planet had at least 4 satellites some
of which remained in their previous orbit, but two of them were dragged towards the sun and were captured by Earth. The
largest became its lonely moon while the second fell on its surface giving origin to the continents. This event happened about
3,96 billion of years ago, as it is proven by the ages of the numerous samples brought from the moon
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.
This document discusses iron isotope measurements of lunar samples, including the oldest lunar rock dunite 72 415. The key points are:
1) Dunite 72 415 has a surprisingly light iron isotope composition, in contrast to other lunar samples which are enriched in heavy iron isotopes compared to Earth.
2) Additional measurements of dunite 72 415 confirm this light iron isotope signature.
3) The earliest olivine accumulation in the lunar magma ocean may have been enriched in light iron isotopes, allowing the overall iron isotope composition of the Moon to match that of Earth.
Predictions of the_atmospheric_composition_of_gj_1132_bSérgio Sacani
GJ 1132 b is a nearby Earth-sized exoplanet transiting an M dwarf, and is amongst the most highly
characterizable small exoplanets currently known. In this paper we study the interaction of a magma
ocean with a water-rich atmosphere on GJ 1132b and determine that it must have begun with more
than 5 wt% initial water in order to still retain a water-based atmosphere. We also determine the
amount of O2
that can build up in the atmosphere as a result of hydrogen dissociation and loss.
We find that the magma ocean absorbs at most ∼ 10% of the O2 produced, whereas more than
90% is lost to space through hydrodynamic drag. The most common outcome for GJ 1132 b from our
simulations is a tenuous atmosphere dominated by O2
, although for very large initial water abundances
atmospheres with several thousands of bars of O2
are possible. A substantial steam envelope would
indicate either the existence of an earlier H2
envelope or low XUV flux over the system’s lifetime. A
steam atmosphere would also imply the continued existence of a magma ocean on GJ 1132 b. Further
modeling is needed to study the evolution of CO2
or N2
-rich atmospheres on GJ 1132 b.
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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This document discusses the potential for large igneous provinces (LIPs) to cause the "heat death" of terrestrial planets through massive volcanic eruptions that overwhelm the climate system. It examines the timing of LIP events on Earth to estimate the likelihood of nearly simultaneous eruptions. Statistical analysis of Earth's LIP record finds that eruptions within 0.1-1 million years of each other are likely. Simultaneous LIPs could have driven Venus into a runaway greenhouse effect like its current state. The timing of LIP events on Earth provides insight into potential past LIP activity on Venus that may have ended its hypothesized earlier temperate climate.
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The 27 Myr periodicity in the fossil extinction record has been con-
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The document describes simulations of a collision between the Moon and a companion moon approximately 1/3 the diameter of the Moon. The simulations found that at the modeled subsonic impact velocity, the companion moon did not form an impact crater but was instead accreted onto the Moon's surface. This added material contributed a hemispheric layer comparable to the extent and thickness of the lunar farside highlands. The collision also displaced the Moon's magma ocean to the opposite hemisphere, potentially explaining the observed concentration of KREEP materials. The findings suggest this late accretion event could explain the geological dichotomy between the lunar near and farside regions.
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1) The document discusses theories of galaxy formation from the early universe following the Big Bang.
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This document provides an overview of the atmospheres of the Jovian planets (Jupiter, Saturn, Uranus, and Neptune). It discusses the composition and structure of their atmospheres based on equilibrium cloud condensation models. The atmospheres contain temperature minima at the tropopause, above which temperatures increase due to absorption of sunlight, and below which temperatures increase with depth due to convection. While early models predicted ammonia and water cloud decks, spacecraft observations have since directly observed ammonia clouds on Jupiter but found they are short-lived, suggesting other cloud composition processes.
Constraints on Ceres’ internal structure and evolution from its shape and gra...Sérgio Sacani
Ceres is the largest body in the asteroid belt with a radius of
approximately 470 km. In part due to its large mass, Ceres more closely approaches
hydrostatic equilibrium than major asteroids. Pre-Dawn mission
shape observations of Ceres revealed a shape consistent with a hydrostatic
ellipsoid of revolution. The Dawn spacecraft Framing Camera has been imaging
Ceres since March 2015, which has led to high-resolution shape models
of the dwarf planet, while the gravity field has been globally determined to
a spherical harmonic degree 14 (equivalent to a spatial wavelength of 211 km)
and locally to 18 (a wavelength of 164 km). We use these shape and gravity
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explained by Airy isostatic compensation mechanism. Different models of isostasy
give crustal densities between 1200 and 1400 kg=m3 with our preferred model
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.
The SPHERE view of three interacting twin disc systems in polarised lightSérgio Sacani
Dense stellar environments as hosts of ongoing star formation increase the probability of gravitational encounters among stellar
systems during the early stages of evolution. Stellar interaction may occur through non-recurring, hyperbolic or parabolic passages
(a so-called ‘fly-by’), through secular binary evolution, or through binary capture. In all three scenarios, the strong gravitational
perturbation is expected to manifest itself in the disc structures around the individual stars. Here, we present near-infrared
polarised light observations that were taken with the SPHERE/IRDIS instrument of three known interacting twin-disc systems:
AS 205, EM* SR 24, and FU Orionis. The scattered light exposes spirals likely caused by the gravitational interaction. On
a larger scale, we observe connecting filaments between the stars. We analyse their very complex polarised intensity and put
particular attention to the presence of multiple light sources in these systems. The local angle of linear polarisation indicates
the source whose light dominates the scattering process from the bridging region between the two stars. Further, we show
that the polarised intensity from scattering with multiple relevant light sources results from an incoherent summation of the
individuals’ contribution. This can produce nulls of polarised intensity in an image, as potentially observed in AS 205.We discuss
the geometry and content of the systems by comparing the polarised light observations with other data at similar resolution,
namely with ALMA continuum and gas emission. Collective observational data can constrain the systems’ geometry and stellar
trajectories, with the important potential to differentiate between dynamical scenarios of stellar interaction.
1) Global climate models that include sophisticated cloud schemes show that tidally locked planets can develop thick water clouds near the substellar point due to strong convection. These clouds greatly increase the planetary albedo and stabilize temperatures, allowing habitability at twice the stellar flux previously thought possible.
2) The cloud feedback is stabilizing, as higher stellar flux produces stronger convection and higher albedos. Substellar clouds can block outgoing radiation, reducing the day-night temperature contrast.
3) Non-tidally locked planets do not experience this stabilizing cloud feedback, as clouds only form over parts of the tropics and mid-latitudes. Their albedo decreases with increasing stellar flux, producing a destabil
A Tale of 3 Dwarf Planets: Ices and Organics on Sedna, Gonggong, and Quaoar f...Sérgio Sacani
The dwarf planets Sedna, Gonggong, and Quaoar are interesting in being somewhat smaller than
the methane-rich bodies of the Kuiper Belt (Pluto, Eris, Makemake), yet large enough to be
spherical and to have possibly undergone interior melting and differentiation. They also reside
on very different orbits, making them an ideal suite of bodies for untangling effects of size and
orbit on present day surface composition. We observed Sedna, Gonggong, and Quaoar with the
NIRSpec instrument on the James Webb Space Telescope (JWST). All three bodies were
observed in the low-resolution prism mode at wavelengths spanning 0.7 to 5.2 μm. Quaoar was
additionally observed at 10x higher spectral resolution from 0.97 to 3.16 μm using mediumresolution gratings. Sedna’s spectrum shows a large number of absorption features due to ethane
(C2H6), as well as acetylene (C2H2), ethylene (C2H4), H2O, and possibly minor CO2.
Gonggong’s spectrum also shows several, but fewer and weaker, ethane features, along with
stronger and cleaner H2O features and CO2 complexed with other molecules. Quaoar’s prism
spectrum shows even fewer and weaker ethane features, the deepest and cleanest H2O features, a
feature at 3.2 μm possibly due to HCN, and CO2 ice. The higher-resolution medium grating
spectrum of Quaoar reveals several overtone and combination bands of ethane and methane
(CH4). Spectra of all three objects show steep red spectral slopes and strong, broad absorptions
between 2.7 and 3.6 μm indicative of complex organic molecules. The suite of light
hydrocarbons and complex organic molecules are interpreted as the products of irradiation of
methane. The differences in apparent abundances of irradiation products among these three
similarly-sized bodies are likely due to their distinctive orbits, which lead to different timescales
of methane retention and to different charged particle irradiation environments. In all cases,
however, the continued presence of light hydrocarbons implies a resupply of methane to the
2
surface. We suggest that these three bodies have undergone internal melting and geochemical
evolution similar to the larger dwarf planets and distinct from all smaller KBOs. The feature
identification presented in this paper is the first step of analysis, and additional insight into the
relative abundances and mixing states of materials on these surfaces will come from future
spectral modeling of these data.
Tidal star-planet interaction and its observed impact on stellar activity in ...Sérgio Sacani
This study investigates tidal star-planet interaction by analyzing X-ray observations of planet-hosting stars that are part of wide binary systems. The study compares the X-ray luminosity, an indicator of stellar activity, between the planet-hosting primary star and its non-planet hosting companion star. By analyzing 34 such binary systems with X-ray data from XMM-Newton and Chandra, the study finds that planet hosts with close-in massive planets have higher X-ray luminosity compared to their companion stars, indicating tidal interaction is altering the rotation and magnetic activity of the host stars. The study concludes tidal interaction from massive, close-in planets can impact the rotational evolution of stars, while more distant or smaller planets likely
The Dynamical Consequences of a Super-Earth in the Solar SystemSérgio Sacani
Placing the architecture of the solar system within the broader context of planetary architectures is one of the
primary topics of interest within planetary science. Exoplanet discoveries have revealed a large range of system
architectures, many of which differ substantially from the solar system’s model. One particular feature of exoplanet
demographics is the relative prevalence of super-Earth planets, for which the solar system lacks a suitable analog,
presenting a challenge to modeling their interiors and atmospheres. Here we present the results of a large suite of
dynamical simulations that insert a hypothetical planet in the mass range 1–10 M⊕ within the semimajor axis range
2–4 au, between the orbits of Mars and Jupiter. We show that, although the system dynamics remain largely
unaffected when the additional planet is placed near 3 au, Mercury experiences substantial instability when the
additional planet lies in the range 3.1–4.0 au, and perturbations to the Martian orbit primarily result when the
additional planet lies in the range 2.0–2.7 au. We further show that, although Jupiter and Saturn experience
relatively small orbital perturbations, the angular momentum transferred to the ice giants can result in their ejection
from the system at key resonance locations of the additional planet. We discuss the implications of these results for
the architecture of the inner and outer solar system planets, and for exoplanetary systems
All astronomical bodies originate inside clouds of gas and dust, therefore there should be a common process that leads to
their condensation. In a galactic cloud there is always a gradient of speeds from point to point. Thanks to it, vortices originate
that rake the material of the surrounding cloud gradually forming large gaseous disks, inside which vortices of second order
develop that concentrate the matter of their orbits forming smaller and much denser disks, within which third order vortices
further concentrate the matter. The dense cores of these vortices finally condense in massive bodies: sun, planets and satellites.
The result should be a well ordered planetary system with no “debris” around and where both planets and satellites obey to
a precise rule of the distances from their central body. The solar system complies with these conditions with three main
exceptions. First, in an orbit where a large planet should be there is only a huge number of scattered asteroids. Second, Earth
and its moon with all evidence were not formed in the same vortex, which means that Moon originated somewhere else. Third,
Neptune’s satellite system has been shattered by the intrusion of a foreign body, Triton, and its largest satellites are missing.
These exceptions seem to be strictly connected to each other and all due to a unique event, that is: Triton has diverted the
largest Neptune satellite towards the Sun. This satellite impacted at high speed against the missing planet, scattering myriads
of fragments from its mantle and pushing it towards the sun, where it eventually fell. The planet had at least 4 satellites some
of which remained in their previous orbit, but two of them were dragged towards the sun and were captured by Earth. The
largest became its lonely moon while the second fell on its surface giving origin to the continents. This event happened about
3,96 billion of years ago, as it is proven by the ages of the numerous samples brought from the moon
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.
This document discusses iron isotope measurements of lunar samples, including the oldest lunar rock dunite 72 415. The key points are:
1) Dunite 72 415 has a surprisingly light iron isotope composition, in contrast to other lunar samples which are enriched in heavy iron isotopes compared to Earth.
2) Additional measurements of dunite 72 415 confirm this light iron isotope signature.
3) The earliest olivine accumulation in the lunar magma ocean may have been enriched in light iron isotopes, allowing the overall iron isotope composition of the Moon to match that of Earth.
Predictions of the_atmospheric_composition_of_gj_1132_bSérgio Sacani
GJ 1132 b is a nearby Earth-sized exoplanet transiting an M dwarf, and is amongst the most highly
characterizable small exoplanets currently known. In this paper we study the interaction of a magma
ocean with a water-rich atmosphere on GJ 1132b and determine that it must have begun with more
than 5 wt% initial water in order to still retain a water-based atmosphere. We also determine the
amount of O2
that can build up in the atmosphere as a result of hydrogen dissociation and loss.
We find that the magma ocean absorbs at most ∼ 10% of the O2 produced, whereas more than
90% is lost to space through hydrodynamic drag. The most common outcome for GJ 1132 b from our
simulations is a tenuous atmosphere dominated by O2
, although for very large initial water abundances
atmospheres with several thousands of bars of O2
are possible. A substantial steam envelope would
indicate either the existence of an earlier H2
envelope or low XUV flux over the system’s lifetime. A
steam atmosphere would also imply the continued existence of a magma ocean on GJ 1132 b. Further
modeling is needed to study the evolution of CO2
or N2
-rich atmospheres on GJ 1132 b.
Similar to Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Material During the Nice Model Migration (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.
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.
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.
Continuum emission from within the plunging region of black hole discsSérgio Sacani
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.
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.
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.
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)”
ESA/ACT Science Coffee: Diego Blas - Gravitational wave detection with orbita...Advanced-Concepts-Team
Presentation in the Science Coffee of the Advanced Concepts Team of the European Space Agency on the 07.06.2024.
Speaker: Diego Blas (IFAE/ICREA)
Title: Gravitational wave detection with orbital motion of Moon and artificial
Abstract:
In this talk I will describe some recent ideas to find gravitational waves from supermassive black holes or of primordial origin by studying their secular effect on the orbital motion of the Moon or satellites that are laser ranged.
PPT on Direct Seeded Rice presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
Current Ms word generated power point presentation covers major details about the micronuclei test. It's significance and assays to conduct it. It is used to detect the micronuclei formation inside the cells of nearly every multicellular organism. It's formation takes place during chromosomal sepration at metaphase.
The technology uses reclaimed CO₂ as the dyeing medium in a closed loop process. When pressurized, CO₂ becomes supercritical (SC-CO₂). In this state CO₂ has a very high solvent power, allowing the dye to dissolve easily.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Material During the Nice Model Migration
1. Draft version May 17, 2024
Typeset using L
A
TEX twocolumn style in AASTeX631
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Material During the
Nice Model Migration
Eva Zlimen,1
Elizabeth Bailey,1
and Ruth Murray-Clay1
1University of California, Santa Cruz
1156 High Street
Santa Cruz, CA 95064, USA
ABSTRACT
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.
1. INTRODUCTION
The Nice model (Tsiganis et al. 2005; Gomes et al.
2005; Morbidelli et al. 2005) is a widely-invoked sce-
nario for solar system formation, which was originally
motivated by the long timescales required to form
Uranus and Neptune at their current locations when gas-
mediated accretion processes are not considered (e.g.
Helled & Bodenheimer 2014). While models of peb-
ble accretion (e.g. Lambrechts & Johansen 2012) can
grow the ice giants quickly (e.g., Frelikh & Murray-Clay
2017), Nice-model type upheaval scenarios remain pop-
ular due to their ability to produce dynamically excited
small body populations in the solar system (e.g., Levison
et al. 2008).
A basic premise of the Nice model is that the four
giant planets started in a much more compact configu-
ration than seen today, with all four residing between
∼5 − 20 au. Jupiter and Saturn start out in a resonant
configuration (e.g., Morbidelli & Crida 2007), which is
disrupted by a chaotic upheaval due to interaction with
a planetesimal disk extending from just beyond the orbit
Corresponding author: Eva Zlimen
ezlimen@ucsc.edu
of the farthest planet to ∼30 au. Uranus and Neptune
sweep through the disk, accreting and scattering plan-
etesimals until dynamical friction brings them to rest
at their approximate present-day positions. Numerical
simulations (e.g. Tsiganis et al. 2005) find that in 50%
of cases, Uranus and Neptune swap their initial orbital
ranks. Whether Uranus and Neptune switched places
is currently considered an open question. A scenario
where Neptune started interior to Uranus’ orbit could
account for its greater mass, as the disk surface density
is understood to decrease with radius (Helled & Fortney
2020).
During this sweeping outward migration proposed by
the Nice model, Uranus and Neptune would have inter-
acted with a substantially massive disk (30 − 50 M⊕)
(Morbidelli & Crida 2007). While the proportion of ma-
terial scattered versus accreted by these planets has been
examined (Matter et al. 2009), the origin within the disk
of these accreted planetesimals has not yet been consid-
ered in detail. To investigate the population of accreted
planetesimals in more depth, we directly simulate col-
lisions between test particles and planets. This is in
contrast to Matter et al. (2009), in which collisions were
computed retroactively using the orbital elements of all
particles at every time step to determine collision prob-
abilities as described by Wetherill (1967). Additionally,
arXiv:2405.09621v1
[astro-ph.EP]
15
May
2024
2. 2
we focus on late-stage accretion, with the inner edge of
our planetesimal disk at a greater radial distance, thus
excluding some planetesimals which may already have
been incorporated into the planets at earlier stages of
formation.
In this work, we derive the extent of late-stage accre-
tion during a Nice model orbital migration using direct
N-body simulations. We investigate whether this “late
veneer” of planetesimal accretion could have contributed
substantial heavy element pollution to the atmosphere
and/or envelope of the ice giants. We determine the rel-
ative differences in accretion expected between the two
ice giants in different migration scenarios, particularly
the two cases where Uranus and Neptune either swap or
maintain their initial order.
The ice giants Uranus and Neptune have broadly
similar physical properties, such as radius, mass, and
mean density. Both planets’ atmospheres are dominated
by hydrogen, helium, and methane (Guillot & Gautier
2015). While a protosolar abundance of helium relative
to hydrogen is consistent with observations of both plan-
ets (Conrath et al. 1991a, 1987), their atmospheres are
enriched in methane by over 50× compared to the pro-
tosolar value (Baines & Smith 1990; Sromovsky et al.
2011; Karkoschka & Tomasko 2011).
Moreover, similar interior structures are generally pre-
dicted for these planets: an exterior H2 dominated en-
velope encasing a heavy-element enriched deep interior
and, in some cases, a separate rocky core (Podolak et al.
1991b; Hubbard et al. 1995; Nettelmann et al. 2013;
Bailey & Stevenson 2021). This comparison of interior
models to the gravitational fields of these planets (Ja-
cobson 2014; Tyler et al. 1989; Lindal 1992) robustly
demonstrates that the envelope of Neptune is signifi-
cantly enriched in heavy elements compared to the en-
velope of Uranus. Due to the intermediate density of
these planets, there is not a unique composition profile
that satisfies the measured gravity fields (e.g. Podolak
et al. 1991a; De Wit & Seager 2013). For the sake of
clarity, it is crucial to note that the “atmosphere” is
generally defined as a relatively thin layer exterior to
the “envelope,” which extends deep into the interior.
In contrast to the dipole-dominated fields of other so-
lar system dynamos, the relatively quadrupole-dominant
fields of Uranus and Neptune (Connerney et al. 1987,
1991) appear to suggest the two ice giants have distinctly
similar interior convection patterns, although various
different scenarios can be implicated in producing this
type of field geometry. A convecting thin shell atop
a stably stratified interior (Stanley & Bloxham 2004,
2006) has been a widely considered scenario. Alterna-
tively, turbulent models (Soderlund et al. 2013) have
also been suggested. Particularly given the distinctly
similar magnetic fields of Uranus and Neptune, it is
widely considered to be a paradox that the observed heat
fluxes of these planets are vastly different. Both Voyager
2 (Conrath et al. 1989, 1991b; Pearl & Conrath 1991)
and ground-based (Loewenstein et al. 1977a,b) measure-
ments have revealed that while Neptune has a significant
heat flux, the heat flux from Uranus is much lower, and
could be consistent with zero given current data, though
an analysis which takes into account the wavelength de-
pendence of Uranus’ Bond albedo, influencing the radi-
ant energy budget, may imply a greater heat flow, as
Li et al. 2018 found in the case of Jupiter. This strik-
ing difference in heat flux suggests Uranus and Neptune
have experienced different thermal history. One of the
leading hypotheses for the low heat flux of Uranus is
that convection in the deep interior is inhibited, pre-
venting heat from being released as rapidly as it would
in a fully adiabatic planet (Podolak et al. 1991b). In
addition, it has been proposed that the discrepancy in
heat flow could be due to boundary layers in Uranus’ in-
terior (Nettelmann et al. 2016) or inhibited convection
either in the deep interior (Podolak et al. 2019) or at-
mosphere and upper envelope (Markham & Stevenson
2021). A low initial temperature for Uranus (Podolak
et al. 1991a), has been suggested as a potential reason
why these planets evolved differently. Alternative expla-
nations include giant impactor(s) prompting convective
mixing in Neptune’s interior or altering the atmospheric
composition of both ice giants (Reinhardt et al. 2020;
Morbidelli et al. 2012; Kegerreis et al. 2018).
Indeed, the thermal evolution of these planets may de-
pend on a variety of effects related to volatile enhance-
ment in the envelopes and atmospheres. For example,
as existing gravity data suggest different water mol frac-
tions in the respective envelopes of these planets (>10%
for Neptune and <1% for Uranus), Bailey & Steven-
son (2021) suggested gradual demixing in the interior
of Neptune but not Uranus may account for the dis-
crepancy in heat flow. Another mechanism suggested to
account for the ice giant heat flow discrepancy is release
of latent heat in the atmosphere and upper envelope
(Kurosaki & Ikoma 2017). In this model, pollution of
the atmosphere and upper envelope by up to a 50% mol
fraction of heavy elements elevates planetary luminosity
through latent heat release by condensation of molecules
such as water, methane, and ammonia. The simultane-
ous effects of convective inhibition and latent heat were
also considered by Markham & Stevenson (2021) for
their potential impact on planetary luminosity due to
water and methane condensation assuming mol fractions
of 5% and 12%, respectively; while methane condensa-
3. 3
tion can shorten the cooling timescale, water condensa-
tion will increase the required time to cool, both by up
to 15%.
In this work, we explore whether upsweep of icy mate-
rial by the ice giants during their long-range Nice model
migration was sufficient to produce the differences in
volatile pollution necessary to account for these pro-
posed effects. In order for these processes to explain the
disparate heat of the ice giants, Uranus and Neptune
must obtain different heavy element enhancements. We
simulate the Nice Model migration and consider this late
dynamical stage as a reason for the two planets’ differ-
ences: Uranus and Neptune take different paths through
the disk, accreting differing amounts of planetesimals of
various compositions. While previous works (Tsiganis
et al. 2005; Batygin & Brown 2010; Levison et al. 2011)
highlighted orbital sculpting of the outer solar system
sculpting in an upheaval event, we focus here on the
resultant impacts on the ice giants. We quantify dif-
ferences in quantity and composition of accreted plan-
etesimals, and the resulting potential for this dramatic
phase of orbital upheaval to affect the composition and
thermal evolution of Uranus and Neptune.
In Section 2, we discuss selecting initial conditions
along with the construction of N-body Nice Model sim-
ulations. We normalize and categorize the varying ac-
cretion histories provided by our simulations in Section
3. We comment on the quantity of heavy elements ac-
creted to the envelope and atmospheres along with the
potential for impacting the thermal evolution of Uranus
and Neptune in Section 4.
2. METHODS
Simulations in this paper used the REBOUND N-
body code (Rein & Liu 2012). The simulations were
integrated using IAS15, a 15th order Gauss-Radau inte-
grator (Rein & Spiegel 2015). We comment on this inte-
grator choice in Appendix A. We identify a set of initial
conditions with Jupiter and Saturn in a 2:3 mean-motion
resonance (MMR) in Section 2.1. A planetesimal disk
was constructed to exclude dynamically cleared parti-
cles in Section 2.2. We discuss migration and damping
forces in Sections 2.3 and 2.4 in lieu of including massive
test particles to prompt a chaotic upheaval. A search for
outcomes resembling our solar system is highlighted in
Section 2.5. The implementation of REBOUND’s IAS15
integrator to preserve reproducibility is discussed in Sec-
tion 2.6.
2.1. Initial Conditions
Jupiter and Saturn were initially placed in a 2:3 MMR
as in Masset & Snellgrove (2001); Morbidelli & Crida
(2007); Pierens & Nelson (2008). Jupiter was initiated
at 5.45 au and Saturn at 7.17 au following Morbidelli &
Levison (2008); Tsiganis et al. (2005); Batygin & Brown
(2010). The semimajor axes of the remaining two giant
planets were randomly varied to find stable simulations.
This was done by selecting from a normal distribution
between 10 and 14.5 au for Uranus and 14.5 and 18
au for Neptune. We assumed as in Morbidelli & Crida
(2007) that the planets came to these positions when the
gas disk was present. While gas disk dispersal can itself
cause dynamical instability, we are interested in Nice-
model-like histories in which the planetary instability is
delayed in time. We therefore integrate our simulations
for 108
years and select initial configurations that are
stable over this timescale.
Because upheaval simulations are chaotic, a single set
of stable initial conditions can be perturbed to gener-
ate a range of representative outcomes. From the set
described above, we pick the simulation in which the
3:2 mean-motion resonance angles for Jupiter and Sat-
urn maintained the tightest resonant libration. The four
giant planets were given eccentricity and inclination of
0.001 as in Tsiganis et al. (2005). As illustrated in Fig-
ure 1, even in the tightest resonant configuration found
by this method, the resonance angles exhibit large libra-
tion amplitudes, which we interpret as coming from the
planets’ initially low eccentrities as well as perturbations
from the other two giant planets. The final planetary
initial conditions are shown in Table 1. We use these
initial conditions for the giant planets in all subsequent
simulations. In what follows, we refer to the simulation
containing only the giant planets initialized with these
initial conditions and employing no additional forces as
the “base simulation.”
2.2. Planetesimal Disk
To determine the inner edge of the planetesimal disk of
test particles, a suite of simulations were run with the
base simulation, with the planetary initial conditions
given in Table 1. Test particles were added on circu-
lar orbits with i = 0◦
and semi-major axes randomly
drawn from a uniform distribution between 5 au and 35
au. Particles were cleared by the stable orbits of the
giant planets after integrating for 3 million years. The
disk was almost completely cleared interior to 20 au and
slightly perturbed interior to 23 au, but relatively unaf-
fected beyond this point, as shown in Figure 2. Based on
this result, the inner edge of the disk was placed at 20 au
in all test cases. The outer edge of the disk was placed at
40 au to maximize potential for accretion by covering the
full range that Neptune may roam into. Truncation of
the solar system’s planetesimal disk at ∼30 au has been
4. 4
Table 1. Initial conditions of the giant planets
Body Semimajor axis (au) Eccentricity Inclination (◦
) True anomaly ϖ Ω Mass (M⊙) Radius (km)
Jupiter 5.45003 0.001 0.001 0 π 0 9.54e-4 6.99e4
Saturn 7.17449 0.001 0.001 π 0 0 2.86e-4 5.82e4
Uranus 10.50767 0.001 0.001 7π /4 π 0 4.50e-5 2.50e4
Neptune 17.6797 0.001 0.001 5π /16 0 0 4.50e-5 2.50e4
ϕ
ϕ ϕ
Figure 1. Jupiter and Saturn were initialized in 3:2 mean motion resonance, with libration angles φJ = 3λS − 2λJ − ϖJ and
φS = 3λS − 2λJ − ϖS where λ refers to the mean longitude and ϖ is the longitude of pericenter. The angle φJ librates around
0 while φS librates around π. Only the first 1 × 105
years are shown for clarity. The ability of the resonance to survive 108
years was used to determine the set of initial conditions used in this simulation (Table 1), which we employ for all subsequent
simulations in this work. The relatively weak and noisy resonant behavior evident here results from inclusion of all four giant
planets as well as the low initial eccentricities of Jupiter and Saturn.
suggested to explain the final semi-major axis of Nep-
tune at the end of its outward migration (Tsiganis et al.
2005; Levison et al. 2008). The initial semi-major axes
of accreted particles found in this work are presented in
Section 3, allowing for straightforward reanalysis of our
results given any choice of truncation radius.
Motivated by observations of protoplanetary disks
(e.g. Andrews et al. 2009), we used a surface density
distribution ∝ r−1
to replicate the expected density of
solids assuming a Nice-model type evolution, consistent
with Morbidelli Crida (2007); Thommes et al. (2008);
Morbidelli Levison (2008); Batygin Brown (2010).
In Section 3.4, we provide the percent of planetesimals
accreted per 2 au band such that a reanalysis of our re-
sults can be performed with any surface density. To con-
struct the modeled planetesimal disk, a rejection method
was employed to choose a random semimajor axis for
each test particle between 20 and 40 au. Since the area
of the disk ∝ r2
, our surface density distribution requires
a probability ∝ r of choosing each randomly drawn semi-
major axis.
Planetesimals were initially given zero eccentricity and
inclination. We drew true anomaly, longitude of ascend-
ing node, and argument of pericenter randomly from a
uniform distribution between 0 and 2π.
2.3. Migration Force
As discussed in Fernandez Ip (1984), exchange of
orbital momentum between planets and planetesimals
would cause Jupiter to migrate inwards and Saturn out-
wards. Since we model planetesimals as test particles
for computational efficiency, we must impose this mi-
gration by hand. A velocity-dependent migration accel-
eration was added to the orbits of Jupiter and Saturn to
move these planets to their current positions, following
Thommes et al. (2008); Morbidelli et al. (2005); Levi-
son et al. (2008). As a result, Jupiter and Saturn leave
their resonance, causing a system-wide upheaval. Our
migration acceleration was derived from
a(t) = af − ∆ae−t/τ
, (1)
where a is the semimajor axis and ∆a is defined as af −
ai, the final minus initial semimajor axes. The migration
timescale is given by τ and t is time in years. This was
motivated to force the gas giants to a predetermined
final semimajor axis, with migration decaying over time
(e.g., Malhotra 1993). To implement this migration, we
add an additional force on Jupiter and Saturn given by
˙
⃗
v =
⃗
v
2a
∆aJ,S
τ
e−t/τ
(2)
5. 5
Figure 2. Test particles were integrated with initial condi-
tions (Section 2.2) to determine the placement of the plan-
etesimal disc. Final vs initial semimajor axes of all test par-
ticles are shown after integration for 3 million years. Planet
initial positions are shown for this non-chaotic simulation.
Test particles (black dots) were almost entirely removed in-
wards of 20 au and thus this was chosen for the inner edge
of the disk. Higher density is shown as darker purple.
where the subscripts J and S apply to Jupiter and Sat-
urn, a and ⃗
v are the semimajor axis and velocity values
at each timestep, and ∆a represents the desired total
change in semimajor axis.
The form of Equation (2) may be understood by
considering a circular orbit. The change in semima-
jor axis required by Equation (1) is ȧ = ∆a
τ e− t
τ . For
a circular orbit, Kepler’s third law may be written
v = (GM∗/a)1/2
so that v̇ = −(1/2)(GM∗/a3
)1/2
ȧ =
−(v/2a)ȧ, where M∗ is the mass of the sun, v is the ve-
locity, and G is the gravitational constant. Combining
these expressions yields the planar components of Equa-
tion (2). The total change in semimajor axis was set
such that Jupiter and Saturn would cease migration at
their present day values. Migration out of the resonance
triggers gravitational upheaval of the ice giants. As the
focus of our study was on the accretionary histories of
Uranus and Neptune post-upheaval, a short migration
timescale for Jupiter and Saturn was chosen for conve-
nience, such that the orbital evolution of the four giant
planets approximately matched those accepted within
the Nice model (e.g. Gomes et al. 2005). Values for the
constants are shown in Table 2.
2.4. Damping Force
Upheaval models rely on dynamical friction between
the planets and planetesimals (Stewart Wetherill
1988) to reduce the eccentricities of the ice giants from
their upheaval values to those observed today. Such
damping is observed in previous works using a massive
planetesimal disk (e.g. Tsiganis et al. 2005, Batygin
Brown 2010). Because computations using massive
planetesimals are expensive, Levison et al. (2008) used
damping forces to replicate the effects of dynamical fric-
tion in their outer solar system upheaval model, which
hosts only test particles. We take a similar approach
here. After the initial chaotic period lasting 105
years
(Table 2), a damping force was added to the simulations,
again such that we obtained a Nice-model type orbital
evolution of the giant planets.
No force can change solely a planet’s eccentricity, e,
without also altering its semi-major axis, so we choose a
damping force that primarily, though not exclusively,
damps eccentricity. This force (per mass) takes the
form1
˙
⃗
v = −
1
τe(1 − e2)
⃗
v −
h
a
θ̂
(3)
where h is the magnitude of the angular momentum vec-
tor ⃗
h = ⃗
r ×⃗
v, and ⃗
r and ⃗
v are the position and velocity
vectors measured with respect to the system’s center of
mass, with magnitudes r and v respectively. The con-
stant τe represents the eccentricity damping timescale
and the semi-major axis a is calculated in the center
of mass frame. We refer to the unit vectors in the
radial and azimuthal directions as r̂ and θ̂. We add
the acceleration given in Equation 3 to our integration
component-by-component in Cartesian coordinates, us-
ing the conversions a = −µ/(v2
− 2µ/r) and e = |⃗
e|,
where µ refers to GMtot, Mtot is the sum of the mass of
the Sun and the mass of the planet undergoing damp-
ing, and the eccentricity vector ⃗
e = −⃗
h × ⃗
v/µ − r̂.
The origin of the acceleration in Equation (3) may be
understood as follows. For a Keplerian orbit, ⃗
v =
(h/a)(1−e2
)−1
h
e sin fr̂ + (1 + e cos f)θ̂
i
, where f is the
object’s true anomaly (Murray Dermott 1999). Dif-
1 This damping reproduces Lee Peale (2002), Figure 4 and
is described in the REBOUND example “Planetary migration
in the GJ876 system (C)” (https://rebound.readthedocs.io/en/
latest/c examples/planetary migration/). Their added accelera-
tion ˙
⃗
v = (2/3)τ−1
e (1 − e2)−1
h
−⃗
v + a−1⃗
h × r̂
i
is equivalent to
Equation (3) except for the factor of 2/3, which may be folded
into τe without changing the functional form.
6. 6
ferentiating this expression with respect to time yields
⃗
v = −
µ
r2
r̂ +
1
2
ȧ
a
⃗
v +
ė
e
1
(1 − e2)
⃗
v −
h
a
θ̂
. (4)
The first term on the right hand side of Equation (4) is
the gravitational acceleration due to the central mass.
If we take ȧ/a = 0 and ė/e = τ−1
e , we recover the added
force in Equation (3). These last choices are not self-
consistent—the change in energy per mass with time,
Ċ, resulting from the acceleration in Equation (3) is not
zero and hence adding this force produces a non-zero ȧ.
However, it may be seen by computing Ċ = ⃗
v · ˙
⃗
v that
the timescale |C/Ċ| = |a/ȧ| on which this force changes
the energy C = −µ/(2a) is longer than |e/ė| ∼ τe by
a factor of order e−1
. Qualitatively, this arises because
⃗
v−(h/a)θ̂ is approximately the orbit’s epicyclic velocity.
Table 2. Force constants
for migration and damping
∆ aJ (au) 0.25
∆ aS (au) -2.36551
τmigration (years) ∼1000
τe(years) 7.5e6
Damping delay (years) 1e5
We comment that
while Fan Batygin
(2017) find that in-
tegrating a full self-
gravitating disk of
planetesimals does
not produce substan-
tially different Nice-
model-type outcomes,
planetesimal-driven
migration and dynamical friction does produce qual-
itative differences from the results we achieve using this
damping term. In particular, both pure planetesimal-
driven migration (Fernandez Ip 1984) and the late-
stage planetesimal-driven stage of a Nice-model-like up-
heaval (Tsiganis et al. 2005) exhibit outward migration
for the ice giants and Saturn, while Jupiter migrates
inward. This behavior results from global exchange
of planetesimals; this is not captured in eccentricity
damping forces, which cause all planets to move inward.
Given the relatively short distance of this migration
in the majority of our models, we do not expect this
difference to substantially affect our results, but we re-
turn to this point in Section 4.5. Dynamical friction
and migration generated by planetesimals is also more
stochastic than modeled here (Murray-Clay Chiang
2006; Nesvornỳ Vokrouhlickỳ 2016; Hermosillo Ruiz
et al. 2023), but this behavior is unlikely to affect the
rate of planetesimal collisions with the ice giants. In
short, the eccentricity damping force employed here
serves the purpose of causing the planets to evolve
qualitatively consistently with the Nice model.
2.5. Simulation procedure
To reduce computational expense, we initially simu-
lated the four giant planets without planetesimals with
the above fictitious forces as in Morbidelli et al. (2005);
Levison et al. (2008); Thommes et al. (2008) in or-
der to determine appropriate migration and damping
timescales. The time that the migration force was ini-
tiated was randomly selected between 100 and 1.5×107
years, acting on the gas giants at different positions in
their orbits. This served to generate a different chaotic
simulation for each selected time. Selected times are
shown in Table 3. As each of these simulations employed
the same initial base simulation that was stable for 108
years we can essentially access all phase space covered by
the planets in just one orbital period. Thus simulations
with shorter times before migration were preferred as
there would be a more complete orbital evolution with
less computational time.
Table 3. Values for
migration delays
Simulation Delay (years)
No Swap 1 443
No Swap 2 392
Swap 1 265
Swap 2 170
We developed a permissive
criterion to determine if sim-
ulations outcomes were simi-
lar to the current solar system
using the percent difference of
the semimajor axes of each
planet, defined as as/ar − 1
where as is the final simulated
semimajor axis and ar is the
real present day axis. An ac-
ceptable simulation was de-
fined as having an average percent difference between
the four planets of less than 8%, with no individual
planet to exceed a percent difference of 20%. Addition-
ally, the eccentricity of each planet must be 0.1.
With our selected timescales, ∼2% of runs had out-
comes which aligned satisfactorily with the current posi-
tions of the ice giants according to our criteria as shown
for four runs in Fig. 3. The remaining 98% had out-
comes that did not remotely resemble that of the so-
lar system: missing an ice giant or having one or more
planets at 40+ au were the most common alternatives,
though there were simulations in which the gas giants
were significantly disrupted from their orbits. The ice
giants swapped positions in approximately half of the
accepted runs, in agreement with Tsiganis et al. (2005).
For convenience, only four simulations were selected to
integrate with test particles, two for each scenario. Full
orbital evolutions for the four chosen runs can be seen in
Fig. 9. These results are consistent with Tsiganis et al.
(2005) and Batygin Brown (2010).
2.6. Reproducibility Modifications
In N-body integrations with many massless test par-
ticles, it is more computationally efficient to run numer-
ous simulations in parallel and compile the data from
all massless particles at the end. Thus, our integra-
7. 7
Figure 3. Simulated mean semimajor axes and eccentricities for each planet (colored rectangles) compared with the corre-
sponding present day values retrieved from JPL Horizons (black dots). Width and height of the rectangles correspond to the
maximum and minimum values of the last 5 million years of the four chosen runs. In two of the runs, Uranus started and ended
interior to Neptune (No Swap 1 and 2) while in the other two Uranus started exterior to Neptune (Swap 1 and 2).
tor needed to be reproducible: for any given set of ini-
tial conditions, the giant planets must follow the same
orbital evolution regardless of the number of massless
bodies present. For non-chaotic simulations, this is gen-
erally not an issue, as the massless bodies by default
do not affect massive bodies. However, due to numer-
ical precision, the addition of these bodies can change
the roundoff error of the force calculations. In chaotic
systems, these errors propagate to the extent that the
outcome of the simulation is substantially affected.
In order to maintain reproducibility in the face of
roundoff errors, the following integration scheme was
implemented. The planetary initial condition archive
file was loaded into a first simulation object to create
a planet-only simulation, which was then copied. Ran-
domly generated massless test particles were added to
the copy, now referred to as the particle simulation. The
planet-only simulation is run for one timestep and then
copied, creating a third simulation object. The parti-
cle simulation is then run to that same time, then the
test particles are copied over into the copied simulation.
The copied simulation now becomes the new particle
simulation. The old particle simulation is freed, and the
process repeats. This ensures that the planetary mo-
tions are only dependent on bodies with mass and are
not being affected by roundoff errors in the timesteps
due to calculations of interactions.
3. RESULTS
We integrated each of the four chosen simulations with
test particles and determine the number of collisions in
Section 3.1. We normalized the simulated test particles
to a standard disk mass in Section 3.2 to obtain the
mass increase for each ice giant, given in Section 3.3.
We determined the formation location of the accreted
planetesimals in Section 3.4. In the following analysis,
Uranus (the final interior ice giant) is always associated
with blue, and Neptune (the final exterior ice giant) with
purple.
3.1. Collisions
Each of the four chosen simulations was integrated
with ∼100,000 test particles in order to get sufficient
statistics on planetesimal accretion. One outcome is
shown in Figure 4; analogous plots for all four chosen
simulations and plots showing the evolution of the plan-
etary orbits over longer timescales are available in Ap-
pendix B. From this, the number of test particle colli-
sions with each planet was acquired for each scenario.
Collisions were detected with REBOUND’s Line detec-
tion module and resolved with a custom collision resolve
function. This recorded the identifying hash of the col-
liding test particle and planet before removing the test
particle from the simulation. Collisions were predomi-
nantly due to particles initially located at the inner edge
8. 8
Figure 4. Semimajor axis (a), apocenter distance a(1+e), and pericenter distance a(1−e) versus time of Jupiter (pink), Saturn
(dark purple), Uranus (blue), and Neptune (light purple) along with the time and location of collisions with test particles for
Uranus (blue triangles) and Neptune (purple stars) during the chaotic period. In this scenario (No Swap 1), the ice giants did
not end with swapped positions: Neptune began and ended exterior to Uranus. Neptune was responsible for ∼80% of the total
test particle collisions.
of the disk, with the outermost ice giant accreting the
majority, as shown in Figure 5. For all simulations,
the majority of collisions occured at the beginning of
the simulation, with collision frequency decreasing with
time.
3.2. Normalization
To convert from the number of collisions that oc-
cur in our simulations to the physical collision rate, we
normalize assuming an initial surface density in plan-
etesimals of 0.25 g/cm2
at 30 au, i.e. surface density
Σp = Σp,0(r/30au)−1
with Σp,0 = 0.25 g/cm2
. As a
result we are simulating a disk in which the total mass
of planetesimals is ∼35M⊕. This is comparable to the
minimum mass solar nebula of Hayashi (1981), using
the density for rock+ice over the same disk radii, and
the disk mass assumed in Desch (2007). Morbidelli
Levison (2008) report that more massive disks did not
provide qualitatively similar outcomes to our solar sys-
tem. We note that the chaotic outcomes of this simu-
lations imply that a large number of simulations would
be required to explore the full phase space of outcomes
for a given disk mass. We used a disk surface den-
sity with a shallower power law than those employed
in Hayashi (1981) and Desch (2007). For a planetesi-
mal surface density ∝ r−1
, our computed rates of mass
accretion onto the planets are linearly proportional to
surface density at 30 au used for normalization. Steeper
profiles would preferentially weight collisions with plan-
etesimals originating near the inner edge of the disk (cf.
Figure 5).
3.3. Mass increase due to accretion
Table 4 summarizes the percent mass increase due to
accretion for three scenarios which each consider differ-
ent regions where accreted planetesimals may be consid-
ered fully ablated and well mixed (discussed in depth in
Section 4). The first scenario assumes the accretion is
well mixed throughout the entire planet (taken as 1029
g)
while the second assumes planetesimals are only mixed
throughout the envelope. The third assumes (small)
planetesimals ablate in the upper envelope and are pre-
vented from mixing with the remainder of the envelope
due to inhibited convection. Entries are presented as the
total final mass in the considered region after accretion
divided by the initial mass. Considered as a percentage
of the total planet mass, the greatest increase was 0.35%
for Neptune in a non-swapping run, with Uranus only
accreting an additional 0.1% of its mass.
Uranus averaged a 0.1% mass increase in all four sce-
narios. For scenarios in which the ice giants swapped,
Neptune averaged a 0.04% mass increase, while for the
9. 9
Figure 5. The left column shows initial locations of accreted
test particles in the disk and the planet they collided with.
The right column gives the total collisions for Uranus (blue)
and Neptune (purple), with the planets identified by their lo-
cations in their final configuration. The first two rows show
simulations in which Uranus initially is exterior to Neptune
(Swaps 12) whereas the bottom two rows show scenarios
in which Neptune starts and ends exterior to Uranus (No
Swaps 12). Collisions are normalized to the total number
undergone by both ice giants in each simulation. The major-
ity of particles were accreted by the initially outermost ice
giant from the inner edge of the disk. The remainder of the
accreted particles originated from all regions of the disk with
little variation.
non-swapping scenarios Neptune’s 0.35% and 0.1% in-
creases were larger. A larger suite of simulations would
be required to fully explore the level of dispersion in out-
comes. Table 4 also provides the enhancement factor by
mass of the planets’ gaseous envelopes, which we take
to comprise 10% of the planets by mass.
3.4. Origin of Accreted Planetesimals
To investigate the origins of planetesimals that ulti-
mately collide with the ice giants, we display the initial
semi-major axes for these planetesimals in Figure 5. In
swapping simulations, Uranus received the most colli-
sions from planetesimals initialized between ∼20 − 24
au. Neptune varied between Swaps 1 and 2, accreting
mostly planetesimals originating in the region ∼36 − 40
au in Swap 1 and ∼25 − 29 in Swap 2. In both, the in-
ner 2-3 au of the planetesimal disk was only accreted by
Uranus. In the non-swapping simulations, Uranus pre-
dominately accreted planetesimals initialized between
24 and 28 au while Neptune mainly collided with plan-
etesimals originating between 20 and 24 au. Notably, in
non-swapping simulations, Uranus accretes a significant
portion of planetesimals formed between 25-38 au while
beginning and ending interior to Neptune. Throughout
all simulations, the average initial semimajor axis of test
particles which collided with Uranus was ∼26 au. For
Neptune, this value was 30 au for swapping scenarios
and 23 au for non-swaps: Neptune accreted test parti-
cles formed farther out in the disk when it was shielded
by an initially exterior Uranus. The initially exterior ice
giant accreted the majority of the inner test particles,
leaving only those farther out for the initially interior
planet. In swapping simulations, the inner 2 − 3 au
of the disk was reserved exclusively for Uranus. How-
ever, while Neptune dominated accretion in this region
in non-swapping scenarios, Uranus was able to accrete
in this area. Thus in both swapping and non swapping
variants, Uranus accretes planetesimals from 20 − 23 au
while Neptune only does so when it is initially exterior.
A discussion of the icelines present in this disk can be
found in Section 4.4.
Both swapping simulations accreted planetesimals
from a similar distribution of initial radii, as did both
non-swapping simulations, as seen in Figure 5. We used
this to determine the impact of our assumed surface den-
sity on the radial collision distribution by summing the
collisions of the two swapping, and, separately, the two
non-swapping simulations. This was normalized to the
initial planetesimal surface density and is displayed in
Figure 6. This provides a way to translate the num-
ber of collisions found to any initial planetesimal surface
density. The accretionary trends apparent in Figure 5
remain visible in Figure 6: the initial chosen surface
density does not greatly influence this result.
10. 10
Table 4. Mass gained due to planetesimal accretion with respect to three regions: the full planet, the envelope, and the upper
envelope to the 100 bar level (total final mass/initial mass)
Simulation Swap 1 Swap 2 No Swap 1 No Swap 2
Planet Uranus Neptune Uranus Neptune Uranus Neptune Uranus Neptune
Total planet mass 1.0011 1.0004 1.0010 1.0003 1.0010 1.0035 1.0009 1.0010
Envelope mass 1.011 1.004 1.010 1.003 1.010 1.035 1.009 1.010
100 bar level mass 7800 2500 7300 2400 7300 27000 7000 7300
Figure 6. Fraction of particles initially located in each 2 au radial bin that ultimately collide with Neptune (purple) and Uranus
(blue). This provides the probability of collision for a given initial test particle semimajor axis, for any initial surface density.
The left plot shows the combined statistics for No Swaps 12 while the right plot shows the same for Swaps 12. Uranus and
Neptune are identified by their locations in their final configuration.
4. DISCUSSION
During the ice giants’ Nice Model migration, we find
that these planets experienced a late accretion of icy
planetesimals equivalent to an envelope mass fraction
of up to ∼3.5%. This phase of solar system formation
would have constituted an extreme bombardment event
for Uranus and Neptune: assuming the majority of the
mass is in km-sized bodies, one of these planets would
have collided with up to 3 planetesimals per hour dur-
ing the first million years of the giant planets’ orbital
instability. Further, the initially exterior ice giant ac-
cretes more planetesimals. We now address the possible
relevance of this substantial impactor flux to the early
thermal evolution of Uranus and Neptune.
As discussed in Section 1, Uranus has a much smaller
present-day observed heat flow than Neptune, despite
the fact that these planets share many outward similar-
ities. We compare our simulations with published mod-
els to evaluate whether the substantial volatile accretion
evident in our simulations could have caused Uranus to
experience rapid cooling compared to Neptune at early
stages of solar system formation after the dispersal of
the gas disk, providing an explanation for the difference
in heat flow. The depth at which planetesimal ablation
occurs determines which part of the planet is affected, so
we consider the full envelope separately from the upper
envelope and atmosphere.
4.1. Comparison to previous work
The extent of accretion undergone by the ice giants
during a Nice model upheaval was considered in Mat-
ter et al. (2009). As mentioned in Section 1, we em-
ployed a collision detection module within REBOUND
to directly simulate collisions between planets and plan-
etesimals instead of determining collisions retroactively
using collision probabilities as utilized by Matter et al.
(2009). In all cases, we find less mass accreted than this
previous work by a factor of 2 to 10 times. It should be
noted that while the total planetesimal disk mass used
by Matter et al. (2009) is comparable to that used in our
work, the disk used in this previous study begins at 15.5
au while our disk begins at 20 au, as we excluded these
dynamically cleared particles assumed to have incorpo-
rated into the planet during earlier planet formation as
discussed in Section 2.2. As the majority of accretion
in our simulations was due to planetesimals at the inner
edge of our disk, we can speculate that including plan-
etesimals interior to 20 au would substantially increase
total accretion relative to the case studied here. Given
this difference, we cannot rule out the possibility that
the N-body and analytical models give different results.
11. 11
However, we do reproduce the finding that the initially
exterior ice giant undergoes the most accretion.
4.2. Heavy element pollution in Uranus and Neptune’s
envelopes
To satisfy gravity observations, models require metal
mole fractions of ≥ 10% and 1% in the envelopes of
Neptune and Uranus, respectively (Bailey Stevenson
2021). Contamination of the envelopes of these plan-
ets by icy planetesimals depends on planetesimal size as
this controls where ablation occurs. Pinhas et al. (2016)
find that icy impactors with radii ∼1 km fall through the
atmosphere and ablate almost entirely by the 1000-bar
level inside the planet due to drag and thermal effects.
Given this finding, it is plausible that 100-km-sized plan-
etesimals would also ablate in the envelope, which ex-
tends to the 105
-bar level (Nettelmann et al. 2013).
Motivated by these ablation levels for large planetesi-
mals, we first consider a scenario in which the accreted
material is mixed by convection throughout a hydrogen-
dominated envelope with 10% of the planet mass (Table
1) (Hubbard MacFarlane 1980).
As mentioned in Section 1, one or more giant im-
pacts have previously been proposed to account for
the observed differences in Uranus and Neptune. We
can consider the accretion examined in our work to be
caused by any plausible planetesimal size-mass distribu-
tion; namely, we can consider the full mass increase and
corresponding change in envelope compositions as being
delivered either over time by many small impactors or
all at once by a ∼1/20M⊕ impactor, the maximum to-
tal accreted mass. We employ the full mass increase for
each planet over the full simulated time, as documented
in Table 4, to obtain the mass gained in volatiles (also
referred to as “metals” or “water”). While it is unre-
alistic to assume the planetesimals are fully water, it
provides a limiting case and allows for direct compari-
son to previously computed models which utilized this
same assumption, such as Kurosaki Ikoma (2017). It
is straightforward to translate the mass accreted that we
find to any planetesimal composition (see Section 4.4 for
an example).
We calculated water mole fractions in the envelopes
due to accretion, with the assumption that the remain-
ing mass of the envelope is a H2-He mixture in solar
proportions (mean molar mass 2.3 g/mol).
Because Uranus and Neptune swapped position in
some simulations but not others, this begs the question
of how these two different migratory outcomes relate to
the amount of material accreted. In all four simulations,
Uranus obtained a ∼0.1% water mole fraction in its en-
velope. As seen in Figure 5, Neptune’s accretion varied
substantially. In the simulation with highest accretion
(No Swap 1), Neptune obtained a volatile mass fraction
of ∼3% in its envelope, corresponding to a ∼0.5% water
mole fraction. In swapping simulations, Neptune only
obtained a water mole fraction of ∼0.04%.
Our enhancements for Uranus were found to be be-
low the limiting value of ∼1%, which, long-term set-
tling notwithstanding, agree with current gravity obser-
vations that suggest Uranus is more centrally condensed
(e.g. Helled et al. 2010; Nettelmann et al. 2013; Podolak
et al. 1995). However, even the case of greatest accre-
tion simulated for Neptune is insufficient to provide the
heavy element enrichment of Neptune observed today.
Accordingly, the substantial difference in heavy element
enrichment of the envelope must have been obtained by
Uranus and Neptune through a different process than
disparate accretion of a “late veneer” as explored in this
work. While volatile enrichment of the envelope during
the Nice model migration was not sufficient to account
for the entire heavy element content of Neptune’s enve-
lope, this late-stage accretion was enough to increase the
mean molecular weight of the envelope by up to ∼3%.
4.3. Heavy element pollution in the atmosphere and
upper envelope
As discussed in Section 1, condensation of water and
methane in the atmosphere and upper envelope may
play a role in the thermal evolution of the ice giants.
Kurosaki Ikoma (2017) find that a 50% water mol
fraction in a young Uranus’ atmosphere and upper en-
velope is sufficient to cool the planet to its observed flux
by present day. Additionally, they find that this lumi-
nosity is almost three orders of magnitude higher than
that due to a 45% mol fraction. Markham Steven-
son (2021) consider the effects on planetary luminos-
ity of stable stratification alongside latent heat release;
they show that while methane condensation increases
luminosity, water condensation causes a longer cooling
timescale.
Accordingly, we consider the possibility that the late
accretion quantified in this work enriched the atmo-
spheres and upper envelopes of the ice giants at early
times, leading to transient but important changes in
cooling. We find that in swapping simulations, Uranus
is enhanced more than Neptune; we sought to quantify
the effect of the excess atmospheric pollution of Uranus.
Following the logic of Kurosaki Ikoma (2017), for the
purposes of this discussion, we assume the mass of the
impactors is entirely in water. Because the mean molec-
ular weights of ammonia and methane are similar to
water, the following conclusions can be loosely applied
to “ices” as a whole. We further follow their approach
12. 12
by considering a region of the planet’s atmosphere and
upper envelope which extends to the 100 bar level.
Small water-ice planetesimals will ablate at or above
this level; in order to consider this scenario, we must
examine the potential for the existence of these small
planetesimals. While ALMA observations show ∼1 mm
planetesimals (often referred to as “pebbles”) present
in gas disks with a collective mass comparable to that
of the minimum mass solar nebula (e.g. Andrews et al.
2009; Andrews 2015), it is unclear if particles of this size
would still be present after disk dispersal. If they were
to remain, collisional grinding would likely reduce the
population of the largest-size pebbles on a timescale of
t = (4/3)(ρints/Σ)Ω−1
. We estimate that a surface den-
sity of pebbles Σ ≳ 5 × 10−6
g cm−2
at 25 au would re-
sult in destruction by collisional grinding over timescales
less than 1 Myr, where we have used an internal pebble
density
ρint = 2 g cm−3
, and Ω is the angular orbital velocity
of a particle at 25 au. Alternatively, if small planetesi-
mals did not survive disk dispersal, they could be formed
through a collisional cascade generated by a reservoir of
1 km bodies. In a classic collisional cascade, the number
of particles at a given size, N(s), has size distribution
dN/ds ∝ s−q
, so that the mass at a given size is propor-
tional to s4−q
. We take q=3.5. For the surface density
discussed in Section 3.2, the time between collisions for
1 km sized objects is ∼20 million years, meaning that
as long as the Nice Model upheaval occurs at least 20
Myr after disk dispersal a collisional cascade is likely
established, well within the ∼800 Myr delay proposed
by Gomes et al. (2005). If this scenario were to occur,
we can expect a small planetesimal surface density of
2.5 × 10−4
g cm−2
in mm-sized objects.
For the remainder of this section, we consider a fidu-
cial surface density of 2.5 × 10−4
g cm−2
of 1 mm plan-
etesimals to get a basic understanding of the potential
implications. This size is small enough to ablate en-
tirely in the atmosphere and upper envelope by the 1
µbar level (Moses 1992). An additional ablation model
would be required to determine the maximum planetes-
imal size to be ablated by the 100 bar level, which could
be a topic of future work.
We normalized simulated collisions following Section
3.2 and consider the mass increase due to accretion in
comparison to the size of the atmosphere. We focus on
the first million years of accretion, when impact rates
were highest. Collision rates peaked at 1015
per hour
(Neptune, No Swap 1), while Uranus averaged 1014
per
hour during this time across all four simulations. We
can expect these small impactors to settle to the en-
velope on timescales of approximately 100 years (Mor-
dasini 2014). Moreover, while not well constrained, the
convective overturn timescale of Neptune has been es-
timated at 100 years (Hubbard 1984). Thus regardless
of whether the impactors were fully or only mostly ab-
lated, they should remain in the atmosphere and upper
envelope at minimum on the order of 100 years.
We estimated the mass of the atmosphere and upper
envelope (∼1022
g) to be a small fraction of the planet
mass, calculated as 4πr2
pγHρp where rp and ρp are the
planetary radius and density, respectively. We deter-
mined ρp at the base of the upper envelope as P/c2
s,
with P as the pressure of 100 bar. The sound speed cs
is calculated as
p
RT/M where R is the gas constant,
T is the temperature (350 K (Mousis et al. 2021)), and
M the mean molar mass of 2.3 g/ml (a solar H2-He
mix). We assumed an adiabatic region with γ ≈ 7/5,
the adiabatic index of H2, as 100 bar is below the gener-
ally expected radiative-convective boundary and there-
fore assumed to be convective. The scale height H was
found as c2
sr2
p/(GMp), where Mp is the planet mass. Us-
ing the mass of the atmosphere and upper envelope, we
determined the water mole fraction of this region due to
planetesimal accretion.
The convective mixing timescale is long enough in
swapping simulations for Uranus’ atmosphere and upper
envelope to accrete ∼6 × 10−5
its original mass, obtain-
ing a water mol fraction of ∼8×10−6
. Neptune gains up
to 0.002 of the mass of its atmosphere and upper enve-
lope in this time, corresponding to a water mol fraction
of ∼10−4
.
However, it is not certain that this region would be
mixed on this 100 year timescale: convective upwelling
or inhibited convection may keep heavy elements aloft.
Interior models of the ice giants can include layers
of inhibited convection beginning at the 200-bar level
(Leconte et al. 2017). For this case, we consider to-
tal accretion over the first million years. Even though
the metallicities that we compute are large enough that
they will likely be subject to overturn instabilities, this
atmospheric enrichment is directly considered, following
Kurosaki Ikoma (2017). Enhancement is much greater
than when considering a 100-year mixing timescale, with
Neptune acquiring up to 25× its atmospheric and upper
envelope mass. (Note that this enhancement is much
smaller than the enhancements provided in Table 4,
which include all of the accreted planetesimal mass, be-
cause we have limited ourselves to the minority of the
mass contained in small pebbles.) For both ice giants
in all modeled scenarios, the volatile mole fractions in
the atmosphere and upper envelope were 0.2, with a
maximum value of 0.8 for Neptune and 0.5 for Uranus.
13. 13
This implies a heavily volatile-enriched atmosphere and
upper envelope.
This enhancement is sufficient to alter the thermal
evolution of the ice giants according to published mod-
els; substantially so in the case of (Kurosaki Ikoma
2017). As mentioned in Section 1, Markham Steven-
son (2021) determine that condensation of methane and
water can alter the cooling timescale by up to 15%, ei-
ther accelerating or lengthening the required time. We
find much higher mol fractions than their assumed 5%
for methane and 12% for water; these were their highest
studied mol fractions and they found that the change
in cooling timescale increased with heavy element con-
centration. We can speculate that this trend will con-
tinue. Without constraining the compositions of wa-
ter and methane in the disk at this time, it is unclear
whether we would expect our simulated planets to un-
dergo an increased (mostly water accreted) or reduced
(mostly methane accreted) cooling timescale. However,
we found that the atmosphere and upper envelope of
the ice giants were flooded with volatiles at early times,
dominating the composition of this region.
For Uranus to experience an accelerated cooling
timescale early in its evolution, we require a swap-
ping simulation in which pebbles are dominantly com-
posed of methane, increasing the planet’s luminosity at
earlier times, thus accelerating its cooling. We found
that Uranus incurred an atmospheric water mol fraction
∼2 times that of Neptune’s in swapping simulations.
Conversely, in non-swapping simulations, Neptune ob-
tained 1.5 times the atmospheric water mole fraction of
Uranus. In a non-swapping scenario, we would require
mainly water to be accreted, causing Neptune’s cool-
ing timescale to increase compared to that of Uranus.
In either case, accretion is significant enough that cool-
ing timescales of both planets would likely simultane-
ously be affected. If the relative amounts of water and
methane in pebbles could be determined during this
time period, we could theorize on the starting configu-
ration of the ice giants. We comment that while pebble
accretion will increase grain input in the upper atmo-
sphere, Mordasini (2014) find that in the outer radiative
zone this increase in dust does not significantly increase
the grain opacity; further, the gas opacity more strongly
effects the thermal evolution (Lunine et al. 1989).
We note that the details of the atmosphere are a key
aspect in dictating how a planet cools over time (e.g.,
Fortney et al. 2011). Fortney et al. (2011) computed at-
mospheric models of Uranus and Neptune in order to de-
termine the thermal evolution, and while they were able
to match Neptune’s known luminosity, they were un-
able to do so for Uranus. This model focused on the at-
mospheric boundary conditions, and highlights the need
for new calculations of atmospheric boundary conditions
for ice giant evolution models, including the possibility
of planetesimal dissolution in the atmosphere. While a
higher opacity may slow cooling, the details of atmo-
spheric opacities are complex. We may expect that the
influx of material associated with planetesimal dissolu-
tion would increase the planet’s opacity, increasing the
solar energy input while decreasing the energy output,
but more updated work is needed to better understand
this feedback.
4.4. N2 and Kr icelines
We now consider the effect of icelines within the plan-
etesimal disk on the atmospheric enhancement of Uranus
and Neptune due to accreted planetesimals. We note
that as Uranus and Neptune began formation in dif-
ferent locations of the disk before undergoing the up-
heaval described in this work, they may have had differ-
ent atmospheric compositions initially. This model only
calculates the enrichment undergone during late-stage
accretion and does not account for any initial metallic-
ity difference. As discussed in Section 4.3, in the case
of a 100-year convective mixing timescale, the metallic-
ity increase due to this accretion is small to moderate
compared to any initial enhancement, and the initial
atmospheric composition would be required to predict
what we observe today. However, in the case of inhib-
ited convection preventing mixing throughout the enve-
lope, enhancement would be dominated by the accretion
explored in this work, and the initial atmospheric com-
position can be neglected. This is true even if the metal-
licity of Neptune’s atmosphere was previously enhanced
to today’s observed value.
As highlighted in Figure 4, the radial source of the
accreted planetesimals varied between swapping and
non-swapping simulations. We considered whether this
difference in planetesimal source populations provides
a measureable compositional signature of whether the
ice giants swapped orientation during a dynamical up-
heaval. Such utility would require a compositional tracer
or tracers that vary across the radial region of the disk
where the planetesimals originate. The N2 iceline at
∼26 au and the krypton (Kr) iceline at ∼22 au (Öberg
Wordsworth 2019) offer perhaps the most promising
possibilities. This model is based on a water snowline
of ∼2 au and a corresponding midplane temperature of
140K, with temperature ∝ r−0.65
. Interior to these ice
lines, N2 and Kr are primarily in gaseous form, while
exterior to the ice lines, they are primarily components
of solid planetesimals and hence are available to be ac-
creted by the ice giants during the collisions described in
14. 14
this work. In particular, in non-swapping scenarios we
may expect krypton (and to a lesser extent, nitrogen)
accretion in Uranus but little to none in Neptune, as
Uranus accretes planetesimals predominately from exte-
rior to 22 au while Neptune accretes from interior to this
radius. In swapping scenarios we may expect enhance-
ment of krypton in both planets while nitrogen accretion
is restricted to Uranus, as both planets accrete planetes-
imals from the 22−26 au region but Neptune’s accretion
is minimal exterior to this. As no carbon icelines exist
within the extent of our disk, carbon is accreted in all
simulations and thus provides a baseline for comparison.
The post-formation enrichments discussed below are
linked to the initial orbital rank of the planets and thus
can be used as a constraint in this respect. To test
this idea, we assigned compositions to the planetesi-
mals in our simulations. Planetesimals were assumed
to have compositions equivalent to the solar nebula with
abundances following Öberg Wordsworth (2019), with
mass split evenly (Greenberg 1998) between silicates and
volatiles such as CO, CO2, ethane, nitrogen, ammonia,
water, and trace noble gases. For the subset of scenar-
ios discussed in Section 4.3, where volatile enrichment
dominates the atmosphere and upper envelope, we find
our prediction is true. As the amount of accretion varies
per simulation, we define fi as the ratio of i:C accreted
by the planet to the solar value of i:C, where i refers to
Kr or N. For krypton, Uranus obtains an approximately
solar enhancement in all simulations (fKr ∼0.9 − 1.1).
In swapping scenarios, Neptune has a solar enrichment
(fKr ∼1.1) while in non-swapping cases this enhance-
ment is subsolar (fKr ∼0.2 − 0.3).
When considering nitrogen enrichment, we find sub-
solar ratios in all cases for Neptune (fN ∼0.1 − 0.3).
In swapping scenarios, Uranus obtains a ∼2 times solar
enhancement while in non-swapping cases enrichment is
subsolar: fN ∼0.6 − 0.8. It is likely that convective
mixing throughout the envelopes of the ice giants has
occurred since this epoch and these minor relative en-
richments will be unable to be detected in their current
atmospheres; however, the resulting enrichment may be
more apparent on the satellites of the ice giants.
4.5. Caveats to the model
Our models employed several simplifications. As dis-
cussed in Section 1, the orbital evolution of the giant
planets during the Nice model evolution has been heav-
ily studied; we sought to replicate this while reducing
computational expense by avoiding the use of massive
test particles. Similar to existing Nice model simula-
tions, we assumed fictional forces to provoke dynamical
instability and to simulate damping caused by dynam-
ical friction. As discussed in Sections 2.3 and 2.4, our
migration force causes Jupiter and Saturn to divergently
migrate, in agreement with models of planetesimal-
driven migration (e.g., Fernandez Ip 1984). However,
we neglect dynamical friction by massive test particles in
favor of our eccentricity damping force, which reduces
the ice giants semimajor axes along with their eccen-
tricities. While reduction of semimajor axis would not
occur with real dynamical friction, our eccentricity force
was made as weak as possible to reduce this effect while
still providing needed damping. The majority of colli-
sions occured during the first million years of the sim-
ulation when semimajor axes, and thus the eccentricity
damping force, were lower. Further, the semimajor axis
space covered by the giant planets during their simu-
lated migration is sufficiently limited such that they are
consistent with published examples of the Nice model
migration. Accordingly, a fictional eccentricity force is
sufficient in place of massive test particles for the pur-
poses of this study.
Moreover, only four different orbital evolution scenar-
ios were simulated in depth. Even with massless test
particles, the computational expense of simulations with
tens of thousands of test particles is high, and we sought
to investigate a few outcomes in detail rather than ob-
tain the complete range of possibilities. We see large
variations in outcomes within our small sample size: in
No Swap 1, total accretion for Neptune was a factor
of 4 higher than either planet in any other scenario.
These simulations provide a starting point to under-
stand accretionary differences between the two scenar-
ios. We would require a large suite each of numerous
orbital evolution scenarios to obtain greater statistics.
Future works could explore the full range of possibilities
in greater detail.
We did not consider the scenario where there are ini-
tially three ice giants (e.g., Batygin et al. 2011; Nesvornỳ
2011). It may be fair to speculate that–as in our
two-planet simulations–the initially outermost ice giant
would accrete the majority of the planetesimals. If this
were the ice giant to be ejected, this could leave less
planetesimals for Uranus and Neptune, preventing as
extreme an impact to their thermal evolution and at-
mospheric compositions. Conversely, if the initially in-
nermost ice giant were ejected, accretion could be simi-
lar to the two ice giant case. However, the three-planet
scenario could benefit from future work, particularly as
observable properties may be concerned.
In addition, we only considered one planetesimal sur-
face density. Proposed planetesimal distributions are
varied (e.g. Weidenschilling 2011; Schlichting et al. 2013;
Johansen et al. 2014), thus we provide estimates at both
15. 15
ends of the size spectrum. Our results can be scaled to
fit any surface density ∝ r−1
. Further, a different func-
tional form of the radial dependence can be investigated
using our results normalized to the initial disk surface
density, available in Figure 6. Ablation depth is depen-
dent on impactor size; we require an additional ablation
calculation to determine the size of impactor that would
ablate by the 100-bar level.
5. CONCLUSION
We have estimated the amount of planetesimal accre-
tion by Uranus and Neptune during the Nice model mi-
gration, investigating how this late stage of accretion
may have impacted the present-day properties of these
planets according to existing models. We carried out
a suite of direct N-body orbital simulations and found
that the ice giants undergo an extreme bombardment
period lasting a million years with mass accretion rates
corresponding to collision rates of up to 3 planetesimals
with 1-km radius per hour. This estimate takes into ac-
count a standard assumption for the surface density of
∝ r−1
with 0.25 g/cm2
at 30 au.
We have found that Uranus and Neptune accrete dif-
fering amounts of volatiles during the Nice model migra-
tion, and specific outcomes vary depending on whether
the planets switch orbital rank. The initially exterior
ice giant accretes the most planetesimals. In simulations
where Uranus is initially exterior to Neptune, both ice
giants accrete planetesimals formed between 22-26 au.
In simulations where Uranus begins and ends interior to
Neptune, Neptune accretes the majority of its planetes-
imals from the inner disk.
When considering the possible role of inhibited con-
vection or convective upwelling in maintaining an ele-
vated fraction of heavy elements in the outer region of
the planet, the atmosphere and upper envelope of the
ice giants down to the ∼100 bar level can be composi-
tionally dominated by the volatiles accreted during this
period. Transient water mol fractions up to 80% are esti-
mated from our orbital simulations. This estimate does
not account for the possibility of hydrodynamic mix-
ing instabilities. If this material exits the atmosphere
and upper envelope on an estimated 100-year convec-
tive timescale, then the metallicity of the planet’s outer
region is not sufficiently enhanced to alter rates of early
thermal evolution. We note that even if inhibited con-
vection or convective upwelling prevent mixing in the
upper envelope and atmosphere during the early ther-
mal evolution of the planets, mixing over the age of the
solar system may have erased enhancements from this
bombardment event that could be observed today.
Future work constraining convective mixing timescales
and regions of inhibited convection in the envelopes
of the ice giants is needed to understand the effect of
volatile accretion on the thermal evolution. Based on
the results of these simulations, we suggest water mol
fractions 0.5 in the upper envelope may have been
temporarily sustained if convection was inhibited below
the atmosphere, as suggested by Leconte et al. (2017).
Crucially, even a brief atmospheric enrichment has the
potential to affect the long-term planetary evolution, as
Kurosaki Ikoma (2017) find a sharp increase of mul-
tiple orders of magnitude in planetary luminosity when
comparing between a 45% and 50% volatile mol frac-
tion in the atmosphere. Accordingly, this work moti-
vates further investigation of the effect of latent heat
release and inhibited convection at water mol fractions
above 50%. The thermodynamic histories and interior
structures of Uranus and Neptune have depended on a
variety of complicated factors over the lifetime of the
solar system. We have established here that these plan-
ets experienced substantial accretion of volatiles from
the massive primordial disk during their long-range out-
ward migration. Accordingly, this late stage of accretion
by Uranus and Neptune deserves further consideration
as a potentially important influence on the observable
properties of these planets.
This work was made possible with funding from the
Heising-Simons Foundation 51 Pegasi b Postdoctoral
Fellowship in Planetary Astronomy and the Undergrad-
uate Research in Science and Technology award from
UC Santa Cruz. We acknowledge use of the lux su-
percomputer at UC Santa Cruz, funded by NSF MRI
grant AST 1828315. We thank Jonathan Fortney and
an anonymous reviewer for helpful comments.
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APPENDIX
A. INTEGRATOR SELECTION
We sought a capable integrator for a chaotic simulation which could accurately resolve close encounters. We imple-
mented a selection scheme for the IAS15 (Rein Spiegel 2015) and Mercurius integrators (Rein et al. 2019) which
involved varying the timestep and switchover parameters of Mercurius and comparing to the IAS15 outcome. We
desired our outcomes to be independent of integrator; however, we found that in this chaotic scenario Mercurius and
IAS15 yielded different results. This type of problem is known to be difficult for symplectic integrators and makes for
an interesting test case.
For each integrator, the four giant planets were initialized in the simulation with randomly selected semimajor axes.
Jupiter’s semimajor axis was selected from between 5.3 and 6 au, with Saturn then placed in a 3:2 MMR following
precedent as in Batygin Brown (2010); Masset Snellgrove (2001); Morbidelli Crida (2007); Pierens Nelson
(2008). We selected a stable multiresonant configuration from Batygin Brown (2010) that was compatible with
a Nice model evolution in which Uranus and Neptune continued the MMR chain, with Uranus in 4:3 MMR with
Saturn and Neptune in a 4:3 MMR with Neptune. The planets were given eccentricities and inclinations of 0.001,
as in Tsiganis et al. (2005). Migration and damping forces were added. Approximately 500 simulations were run for
each set of integrator parameters, and orbital elements over time were saved for each. From these, 2000 timepoints
from all the simulations were randomly selected and plotted on a density distribution as shown in Figure 7. For the
Mercurius integrator, we tested varying the Hill factor parameter (the radius at which the integrator switches from
WHFast to IAS15 to resolve a close encounter) along with the minimum timestep. Our default WHFast timestep was
0.0002 of Jupiter’s period, which ranged from 0.015 to 0.018 in simulation time units (∼ 0.002 years) depending on
the initial semimajor axis. This is an order of magnitude larger than the minimum orbital time for an encounter,
estimated by the period of a body orbiting the at the surface of Jupiter. We also compared our timestep to the
crossover time, the time required to traverse the three hill radii crossover radius rc. We estimated this as rc/(evk),
where the eccentricity e was set to 0.4 and vk is the keplerian velocity, finding ∼ 1 year for Jupiter. The minimum
IAS timestep for close encounters was set to 0.001 of the default WHFast timestep, which is well within the minimum
encounter time and the crossover time. We found that the density distributions for IAS15 and Mercurius were not
consistent with each other. Increasing the Hill factor improved the consistency between the two; however, the Hill
factor needed negated the purpose of using a hybrid integrator, as the integration would fall entirely in the adaptive
timestep regime. Reducing the WHFast timestep did not lead to significant improvement in consistency between the
Mercurious and IAS15 outcomes. It appeared that in this chaotic system the Mercurius hybrid integrator was not
identifying sufficient close encounters. As a result, we elected to use IAS15 for our integrations.
€
Figure 7. Semimajor axis-eccentricity density plots for Neptune representing the evolution of a chaotic system as simulated
with different integrators. For each integrator, 500 simulations were run with orbital elements recorded every 1000 years. The
orbital elements across all 500 simulations were compiled for each planet into one large pool of data. From this, 2000 points
were randomly selected (black dots), so that we were sampling from a range of all simulations. The end result is the distribution
at any given time, with increasing density as darker purple. This compares REBOUND’s IAS15 with the Mercurius default
(Hillfactor = 3), and adjusted to a larger switchover radius (Hillfactor = 7).
19. 19
B. ADDITIONAL FIGURES
Figure 8. Semimajor axis (a), apocenter distance a(1 + e), and pericenter distance a(1 − e) vs time of Jupiter (pink), Saturn
(dark purple), Uranus (blue), and Neptune (light purple) along with the time and location of collisions with test particles for
Uranus (blue triangles) and Neptune (purple stars) during the initial chaotic period. The first row shows simulations in which
Neptune starts and ends exterior to Uranus (No Swaps 12) while the second row shows simulations in which Neptune starts
interior to Uranus (Swaps 12).
Figure 9. Semimajor axis (a), apocenter distance a(1 + e), and pericenter distance a(1 − e) vs time of Jupiter (pink), Saturn
(dark purple), Uranus (blue), and Neptune (light purple) for the full orbital evolution of the four chosen simulations. The
first row shows simulations in which Neptune starts and ends exterior to Uranus (No Swaps 12) while the second row shows
simulations in which Neptune starts interior to Uranus (Swaps 12). Note the differing timescales between plots.