The document describes a study that used laser altimetry from the MESSENGER spacecraft to create a topographic model of Mercury's northern hemisphere. The study found that Mercury has a much smaller range of elevations compared to Mars or the Moon, likely due to Mercury's higher density and gravitational acceleration smoothing out topographic features. The model revealed numerous large impact structures that influence the shape of the hemisphere but do not significantly affect the distribution of elevations.
Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and...Sérgio Sacani
Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the formation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral
Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid
(101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo. The number of boulders is surprising given
Bennu’s moderate thermal inertia, suggesting that simple models linking thermal inertia to particle size do not adequately capture the complexity relating these properties. At the same time, we find evidence for a wide range of particle sizes with distinct
albedo characteristics. Our findings imply that ages of Bennu’s surface particles span from the disruption of the asteroid’s parent body (boulders) to recent in situ production (micrometre-scale particles).
Shape of (101955) Bennu indicative of a rubble pile with internal stiffnessSérgio Sacani
The shapes of asteroids reflect interplay between their interior properties and the processes responsible for their formation
and evolution as they journey through the Solar System. Prior to the OSIRIS-REx (Origins, Spectral Interpretation, Resource
Identification, and Security–Regolith Explorer) mission, Earth-based radar imaging gave an overview of (101955) Bennu’s
shape. Here we construct a high-resolution shape model from OSIRIS-REx images. We find that Bennu’s top-like shape, considerable macroporosity and prominent surface boulders suggest that it is a rubble pile. High-standing, north–south ridges that
extend from pole to pole, many long grooves and surface mass wasting indicate some low levels of internal friction and/or cohesion. Our shape model indicates that, similar to other top-shaped asteroids, Bennu formed by reaccumulation and underwent
past periods of fast spin, which led to its current shape. Today, Bennu might follow a different evolutionary pathway, with an
interior stiffness that permits surface cracking and mass wasting.
Subsurface Determination Of Cavities In Limestone Rock Area By Geoelectric Me...IJERA Editor
Two Dimensional of geoelectric method can be used to find out the conductive formation in the earth surface. The purpose of this research is to give the description about the geological subsurface formation, that the high resistivity value is indicate the potential area of cave and void in the limestone rocks. The dipole dipolegeoelectric method is used in this research with the path of lines is 250 m with 10 m electrode spacing. The total lines is 7 and the azimuth is from east to west. Resistivity method is started with inject the electrical current into the earth by current electrode, then potential difference will arise and measured by potential electrode. Variation value of resistance for each layer rock can calculated by divided potential defference with current value. The existence of the cavity is known by the resistivity value is more than 2500 ohm-m, while the cracks have a resistivity of 1500 to 2500 ohm-m.
Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and...Sérgio Sacani
Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the formation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral
Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid
(101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo. The number of boulders is surprising given
Bennu’s moderate thermal inertia, suggesting that simple models linking thermal inertia to particle size do not adequately capture the complexity relating these properties. At the same time, we find evidence for a wide range of particle sizes with distinct
albedo characteristics. Our findings imply that ages of Bennu’s surface particles span from the disruption of the asteroid’s parent body (boulders) to recent in situ production (micrometre-scale particles).
Shape of (101955) Bennu indicative of a rubble pile with internal stiffnessSérgio Sacani
The shapes of asteroids reflect interplay between their interior properties and the processes responsible for their formation
and evolution as they journey through the Solar System. Prior to the OSIRIS-REx (Origins, Spectral Interpretation, Resource
Identification, and Security–Regolith Explorer) mission, Earth-based radar imaging gave an overview of (101955) Bennu’s
shape. Here we construct a high-resolution shape model from OSIRIS-REx images. We find that Bennu’s top-like shape, considerable macroporosity and prominent surface boulders suggest that it is a rubble pile. High-standing, north–south ridges that
extend from pole to pole, many long grooves and surface mass wasting indicate some low levels of internal friction and/or cohesion. Our shape model indicates that, similar to other top-shaped asteroids, Bennu formed by reaccumulation and underwent
past periods of fast spin, which led to its current shape. Today, Bennu might follow a different evolutionary pathway, with an
interior stiffness that permits surface cracking and mass wasting.
Subsurface Determination Of Cavities In Limestone Rock Area By Geoelectric Me...IJERA Editor
Two Dimensional of geoelectric method can be used to find out the conductive formation in the earth surface. The purpose of this research is to give the description about the geological subsurface formation, that the high resistivity value is indicate the potential area of cave and void in the limestone rocks. The dipole dipolegeoelectric method is used in this research with the path of lines is 250 m with 10 m electrode spacing. The total lines is 7 and the azimuth is from east to west. Resistivity method is started with inject the electrical current into the earth by current electrode, then potential difference will arise and measured by potential electrode. Variation value of resistance for each layer rock can calculated by divided potential defference with current value. The existence of the cavity is known by the resistivity value is more than 2500 ohm-m, while the cracks have a resistivity of 1500 to 2500 ohm-m.
This presentation provides an overview of NASA's Science Mission Directorate that carries out the agency's missions for Earth science, heliophysics, astrophysics, and planetary sciences.
http://science.nasa.gov/
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...Sérgio Sacani
The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy
was the construction of an observatory capable of characterizing habitable worlds. In this paper series
we explore the detectability of and interference from exomoons and exorings serendipitously observed
with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting
in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems
viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every
star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events
per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI)
lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive
the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable
with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain
detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet
features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm
water band where large moons can outshine their host planet, will aid in differentiating exomoon signals
from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin
to our Moon are more likely to be detected in younger systems, where shorter orbital periods and
favorable geometry enhance the probability and frequency of mutual events.
Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...Sérgio Sacani
Mars is a particularly attractive candidate among known astronomical objects
to potentially host life. Results from space exploration missions have provided
insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to
its toxicity. However, it can also provide potential benefits, such as producing
brines by deliquescence, like those thought to exist on present-day Mars. Here
we show perchlorate brines support folding and catalysis of functional RNAs,
while inactivating representative protein enzymes. Additionally, we show
perchlorate and other oxychlorine species enable ribozyme functions,
including homeostasis-like regulatory behavior and ribozyme-catalyzed
chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or
subsurface oxychlorine brines, and brines found in potential lifeforms, could
provide a unique niche for biomolecular evolution.
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.
X-rays from a Central “Exhaust Vent” of the Galactic Center ChimneySérgio Sacani
Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of
linear X-ray-emitting features located within the southern portion of the Galactic center chimney,
and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08◦
, b = −1.42◦
. The
surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may
have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the
feature’s spectra favor a complex two-component model consisting of thermal and recombining plasma
components, possibly a sign of shock compression or heating of the interstellar medium by outflowing
material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this
plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a
sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy
source to sustain the observed morphology
Slack (or Teams) Automation for Bonterra Impact Management (fka Social Soluti...Jeffrey Haguewood
Sidekick Solutions uses Bonterra Impact Management (fka Social Solutions Apricot) and automation solutions to integrate data for business workflows.
We believe integration and automation are essential to user experience and the promise of efficient work through technology. Automation is the critical ingredient to realizing that full vision. We develop integration products and services for Bonterra Case Management software to support the deployment of automations for a variety of use cases.
This video focuses on the notifications, alerts, and approval requests using Slack for Bonterra Impact Management. The solutions covered in this webinar can also be deployed for Microsoft Teams.
Interested in deploying notification automations for Bonterra Impact Management? Contact us at sales@sidekicksolutionsllc.com to discuss next steps.
Connector Corner: Automate dynamic content and events by pushing a buttonDianaGray10
Here is something new! In our next Connector Corner webinar, we will demonstrate how you can use a single workflow to:
Create a campaign using Mailchimp with merge tags/fields
Send an interactive Slack channel message (using buttons)
Have the message received by managers and peers along with a test email for review
But there’s more:
In a second workflow supporting the same use case, you’ll see:
Your campaign sent to target colleagues for approval
If the “Approve” button is clicked, a Jira/Zendesk ticket is created for the marketing design team
But—if the “Reject” button is pushed, colleagues will be alerted via Slack message
Join us to learn more about this new, human-in-the-loop capability, brought to you by Integration Service connectors.
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Generating a custom Ruby SDK for your web service or Rails API using Smithyg2nightmarescribd
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Neuro-symbolic (NeSy) AI is on the rise. However, simply machine learning on just any symbolic structure is not sufficient to really harvest the gains of NeSy. These will only be gained when the symbolic structures have an actual semantics. I give an operational definition of semantics as “predictable inference”.
All of this illustrated with link prediction over knowledge graphs, but the argument is general.
Securing your Kubernetes cluster_ a step-by-step guide to success !KatiaHIMEUR1
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Topography of northern_hemisphere_of_mercury_from_messenger_altimeter
1. Topography of the Northern Hemisphere of Mercury from
MESSENGER Laser Altimetry
Maria T. Zuber et al.
Science 336, 217 (2012);
DOI: 10.1126/science.1218805
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2. REPORTS
References and Notes 14. M. T. Zuber et al., Science 287, 1788 (2000). 27. S. A. Hauck II, A. J. Dombard, R. J. Phillips, S. C. Solomon,
1. S. C. Solomon, R. L. McNutt Jr., R. E. Gold, D. L. Domingue, 15. J. W. Head et al., Science 333, 1853 (2011). Earth Planet. Sci. Lett. 222, 713 (2004).
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10.1126/science.1218805. (2004). Acknowledgments: The MESSENGER project is supported by
4. P. M. Muller, W. L. Sjogren, Science 161, 680 18. J.-L. Margot, S. J. Peale, R. F. Jurgens, M. A. Slade, the NASA Discovery Program under contracts NAS5-97271
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5. D. E. Smith et al., J. Geophys. Res. 98, 20871 (1993). 19. S. J. Peale, Nature 262, 765 (1976). NASW-00002 to the Carnegie Institution of Washington. We
6. D. E. Smith et al., Icarus 209, 88 (2010). 20. S. J. Peale, R. J. Phillips, S. C. Solomon, D. E. Smith, acknowledge the contributions of the MESSENGER spacecraft
7. J. D. Anderson, J. Palguta, G. Schubert, Abstract P41A-1572, M. T. Zuber, Meteorit. Planet. Sci. 37, 1269 team and the radio science and MLA instrument teams in
paper presented at the American Geophysical Union Fall (2002). acquiring the observations used herein. We are also grateful
Meeting, San Francisco, CA, 5 to 9 December 2011. 21. M. Yseboodt, J.-L. Margot, Icarus 181, 327 (2006). to three anonymous reviewers for comments that improved
8. L. R. Nittler et al., Science 333, 1847 (2011). 22. J.-L. Margot, S. Padovan, S. J. Peale, S. C. Solomon, the manuscript.
9. L. R. Nittler et al., Abstract 142-3, paper presented at Abstract P41A-1573, paper presented at the American
the Geological Society of America Annual Meeting, Geophysical Union Fall Meeting, San Francisco, Supporting Online Material
Minneapolis, MN, 9 to 12 October 2011. CA, 5 to 9 December 2011. www.sciencemag.org/cgi/content/full/science.1218809/DC1
10. B. Charlier, T. L. Grove, M. T. Zuber, Lunar Planet. Sci. 23. S. A. Hauck II, S. C. Solomon, D. A. Smith, Geophys. Res.
Materials and Methods
43, abstract 1400 (2012). Lett. 34, L18201 (2007). Figs. S1 to S7
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(2004). 25. G. Morard, T. Katsura, Geochim. Cosmochim. Acta 74, 6 January 2012; accepted 5 March 2012
13. G. A. Neumann, M. T. Zuber, D. E. Smith, F. G. Lemoine, 3659 (2010). Published online 21 March 2012;
J. Geophys. Res. 101 (E7), 16841 (1996). 26. U. R. Christensen, Nature 444, 1056 (2006). 10.1126/science.1218809
or Mars (30 km) (6, 7). Mercury contains nu-
Topography of the Northern merous large impact structures (8, 9) that influ-
ence the hemispheric shape but do not markedly
Hemisphere of Mercury from affect the hypsometry.
Mercury’s high bulk density, presumably the
MESSENGER Laser Altimetry result of an iron-rich core that constitutes an un-
usually large mass fraction of the planet (10),
Maria T. Zuber,1* David E. Smith,1 Roger J. Phillips,2 Sean C. Solomon,3 Gregory A. Neumann,4 yields a surface gravitational acceleration com-
Steven A. Hauck II,5 Stanton J. Peale,6 Olivier S. Barnouin,7 James W. Head,8 parable to that of Mars for a body intermediate in
Catherine L. Johnson,9 Frank G. Lemoine,4 Erwan Mazarico,1,4 Xiaoli Sun,4 Mark H. Torrence,4,10 size between Mars and the Moon. For at least
Andrew M. Freed,11 Christian Klimczak,3 Jean-Luc Margot,12 Jürgen Oberst,13 Mark E. Perry,7 some topography-producing forces, a higher grav-
Ralph L. McNutt Jr.,7 Jeffrey A. Balcerski,5 Nathalie Michel,5 Matthieu J. Talpe,1 Di Yang1 itational acceleration results in less variation in
elevation, which can account for the difference
Laser altimetry by the MESSENGER spacecraft has yielded a topographic model of the northern in topographic dynamic range between Mercury
hemisphere of Mercury. The dynamic range of elevations is considerably smaller than those of Mars and the Moon. However, Mercury’s shallow
or the Moon. The most prominent feature is an extensive lowland at high northern latitudes that core-mantle boundary, at a depth of <400 km
hosts the volcanic northern plains. Within this lowland is a broad topographic rise that experienced below the surface (4), could have affected vis-
uplift after plains emplacement. The interior of the 1500-km-diameter Caloris impact basin cous flow in Mercury’s mantle and may have
has been modified so that part of the basin floor now stands higher than the rim. The elevated influenced the growth and relaxation of the
portion of the floor of Caloris appears to be part of a quasi-linear rise that extends for largest structures (11). Shield-building volcanism
approximately half the planetary circumference at mid-latitudes. Collectively, these features and large-scale extension contribute substantially
imply that long-wavelength changes to Mercury’s topography occurred after the earliest phases to the dynamic range of topography on Mars but
of the planet’s geological history. have no evident counterparts on Mercury. Indeed,
1
he topography of a planet provides fun- mination of MESSENGER’s orbit. Radius is then Department of Earth, Atmospheric and Planetary Sciences,
T damental information about its internal
structure and geological and thermal evo-
lution. Ranging observations made from orbit by
converted to topography (Fig. 1A) by subtracting
the radius of the gravitational equipotential
or geoid obtained from Doppler tracking of
Massachusetts Institute of Technology, Cambridge, MA 02139,
USA. 2Planetary Science Directorate, Southwest Research In-
stitute, Boulder, CO 80302, USA. 3Department of Terrestrial
Magnetism, Carnegie Institution of Washington, Washington,
the Mercury Laser Altimeter (MLA) (1) on the MESSENGER (4). The radial precision of indi- DC 20015, USA. 4NASA Goddard Space Flight Center, Greenbelt,
MErcury Surface, Space ENvironment, GEo- vidual measurements is <1 m, and the accuracy MD 20771, USA. 5Department of Earth, Environmental and
Planetary Sciences, Case Western Reserve University, Cleveland,
chemistry, and Ranging (MESSENGER) (2) with respect to Mercury’s center of mass is OH 44106, USA. 6Department of Physics, University of California,
spacecraft have provided a precise, geodetically better than 20 m (Table 1). MLA can success- Santa Barbara, CA 93106, USA. 7Johns Hopkins University
referenced topographic model of the northern fully range at distances up to 1500 km from Applied Physics Laboratory, Laurel, MD 20723, USA. 8Depart-
hemisphere of the planet as well as a character- Mercury’s surface when operating at nadir, and ment of Geological Sciences, Brown University, Providence, RI
02912, USA. 9Department of Earth and Ocean Sciences, Uni-
ization of slopes and surface roughness over a from ~1000 km at angles up to 40° from the versity of British Columbia, Vancouver, BC V6T 1Z4, Canada.
range of spatial scales. vertical (5). As of 2 December 2011, more than 10
Stinger Ghaffarian Technologies Inc., 7701 Greenbelt Road,
From MESSENGER’s eccentric, near-polar 4.3 million independent measurements of surface Greenbelt, MD 20770, USA. 11Department of Earth and Atmo-
orbit (2), the MLA (3) illuminates surface areas elevation had been obtained. spheric Sciences, Purdue University, West Lafayette, IN 47907,
USA. 12Department of Earth and Space Sciences, University
averaging between 15 and 100 m in diameter, Elevations in Mercury’s northern hemisphere
of California, Los Angeles, CA 90095, USA. 13Institute of Plan-
spaced ~400 m apart along the spacecraft ground exhibit an approximately symmetric, unimodal etary Research, German Aerospace Center, Berlin D-12489,
track. The range from the spacecraft to the sur- hypsometric distribution and a dynamic range Germany.
face is converted to a measurement of radius of 9.85 km (Fig. 2), considerably less than the *To whom correspondence should be addressed. E-mail:
from the planet’s center of mass via the deter- global dynamic range for the Moon (19.9 km) zuber@mit.edu
www.sciencemag.org SCIENCE VOL 336 13 APRIL 2012 217
3. REPORTS
Downloaded from www.sciencemag.org on September 21, 2012
Fig. 1. (A) Polar stereographic projection of topography (local radius minus the projection of median differential slope (15) on a baseline of length 3.2 km, from
radius of the HgM002 geoid, the gravitational equipotential referenced to the the north pole to 50°N latitude. The green line shows the mapped boundary of the
mean equatorial radius) (4) from the north pole to 5°S. The locations of selected northern smooth plains (16); the black line corresponds to the topographic
major impact structures are shown as black circles. (B) Polar stereographic contour of –1.24 km. Both maps include data collected through 24 October 2011.
if the topography associated with Tharsis and Table 1. Geodetic parameters for Mercury derived from MLA topography.
Valles Marineris is excluded, the dynamic range
of the remaining topography on Mars can be Parameter Value
approximated by the rim-to-floor depth of the Reference radius (km) 2440
Hellas basin. This figure is comparable to the North polar radius (km)* 2437.57 T 0.01
dynamic range of topography on Mercury and Equatorial mean radius (km)† 2439.83 T 0.05
is consistent with a gravitational influence on Northern hemisphere mean radius (km)‡ 2439.59 T 0.05
topographic relief for terrestrial planetary bodies. Shape dynamic range (km) 9.848
A spherical harmonic fit of planetary shape Shape accuracy (m) T25
(12) (table S1) confirms an elliptical form of the High point (km)§ 11.222°N, 164.752°E +4.024
equator, with a long axis close to the prime me- Low points (km)§
ridian (12) (fig. S1), as well as an offset between Rachmaninoff, 27.417°N, 57.215°E – 5.815
the center of mass and center of figure in the Polar crater, 85.446°N, 62.440°E – 5.824
equatorial plane (5, 13). This distinctive feature Hypsometric mean (km)§ – 0.589
of the planetary shape reflects a hemispheric Hypsometric median (km)§ – 0.616
difference in internal structure that could poten- Hypsometric mode (km)§ – 0.700
tially arise from large-scale variations in crustal (a – b)/a || (514 T 52) × 10−6
thickness or density, mantle density, or topography f2 (°E)# –18.6 T 4
along Mercury’s core-mantle boundary. CoF-CoM x (km)** 0.133 T 0.052
A north-polar projection of topography CoF-CoM y (km)** 0.193 T 0.051
(Fig. 1A) shows irregular lowlands at high *Average of all MLA observations within 10° of north pole. †Average of all MLA observations within 15° of equator. ‡Mean
northern latitudes that are ~2 km deeper than planetary radius from a spherical harmonic least-squares fit to all observations with a Kaula constraint applied. §Relative to
the surrounding terrain. Portions of the boundary the reference radius. ||a and b are, respectively, the semimajor and semiminor axes of the ellipse fit to shape measurements
within 15° of the equator. #Longitude of the equatorial semimajor axis of the ellipse fit to near-equatorial shape. Longitude
of the northern lowlands appear to follow seg- 0° coincides with one of the hot poles of Mercury, which is on the axis of minimum moment of inertia, and 90° on the equator
ments of rims of degraded impact basins, but the is in the direction of the intermediate axis of inertia. **CoF-CoM is the offset of the center of figure (CoF) from the center of
large extent of the lowlands and the irregular mass (CoM), the origin of the coordinate system for gravity and topography; x and y are the components of offset in Mercury’s
equatorial plane in the direction of 0° and 90°E, respectively.
shape of the remainder of the boundary suggest
that additional processes were involved in the
formation of relief. The northern lowlands are topographic support from flexural and mem- cipal inertia axes driven by the shallow mass
marked by a negative free-air gravity anomaly brane stresses. Barring some sort of offsetting deficit (14). If the present location of the northern
and are in a state of approximate local compen- structure near the south pole, the large area of lowlands is a consequence of polar wander, then
sation (e.g., underlain by thinner than average low topography at high latitudes raises the pros- the implied planet-scale reorientation must have
crust) (4), although the area is likely not in strict pect that the region may have migrated to the occurred at a time when the outer portions of
local mass balance because of contributions to pole during a reorientation of the planet’s prin- Mercury were sufficiently cool and mechanical-
218 13 APRIL 2012 VOL 336 SCIENCE www.sciencemag.org
4. REPORTS
ly strong to preserve a nonhydrostatic response Spectrometer (XRS) indicate that the northern ular, the northern lowlands host a regional
to topographic stresses, as well as the present plains are similar in composition to basalts on topographic rise (centered near 68°N, 33°E)
configuration of inertial axes. other terrestrial bodies (17, 18). The diameters that is ~950 km in diameter and is elevated by
A map of median differential slope (15) of partially to fully buried craters on the plains ~1.5 km above its surroundings. This northern
derived from the topographic measurements unit imply that plains thicknesses, at least lo- rise is characterized by a large (~150 mGal)
(Fig. 1B) illustrates that kilometer-scale slopes cally, exceed 1 to 2 km (16). The black curve positive gravity anomaly (4). This value is only
are generally much lower within the northern in Fig. 1B shows that the boundary of the slightly less than the magnitude of the anomaly
lowlands than in the surrounding areas. The low- smoothed plains and of the area of low dif- that would be predicted by topography alone and
lands are partially filled with a smooth plains ferential slope is reasonably well matched along suggests at most limited compensation (e.g., by
unit that occupies more than 6% of Mercury’s a substantial portion of its length by a constant thickened crust) (4). The northern rise does not
surface (16). On the basis of its geological char- elevation relative to the geoid. These relation- display kilometer-scale slopes distinguishable
acteristics, the plains have been interpreted as a ships suggest that the flood volcanism that from the rest of the northern plains (Fig. 1B),
product of flood volcanism early in Mercury’s created the northern plains involved highly fluid and the size-frequency distributions of super-
history marked by high rates of eruption of high- lavas. posed impact craters indicate that the age of
temperature lavas (16). Elemental composition At present, however, the northern smooth the rise surface is indistinguishable from that
measurements made with MESSENGER’s X-Ray plains deviate from a level surface. In partic- of the surrounding plains (19). Moreover, topo-
graphic profiles through volcanically buried
Fig. 2. Histogram of northern craters on the rise indicate that the flooded
Downloaded from www.sciencemag.org on September 21, 2012
hemisphere elevations, relative floors tilt away from the highest point on the
to a sphere of radius 2440 km, rise (20). These observations indicate collective-
projected onto an equal-area ly that at least a portion of the rise topography
grid from 4°S to 83.5°N. The postdates the emplacement of the plains. The
red line is a smooth curve fit implied vertical motions following plains em-
to the observations; the red placement could be the result of lithospheric
bar indicates T1 standard de- deformation, magmatic intrusion, or mantle dy-
viation from the mean. namic uplift.
The Caloris basin (centered at 31°N, 160°E),
1550 km in diameter (21), is the best preserved
and presumably youngest of the large impact
basins on Mercury (8, 22). A terrain model of
the Caloris region derived from stereo images
acquired during MESSENGER’s first Mercury
flyby (23) displayed basin-concentric rings and
suggested long-wavelength undulations of the
basin interior surface, but the lack of long-
wavelength geodetic control in the model ren-
dered these undulations uncertain. The MLA
Fig. 3. (A) Average along-track tilts of the floors of impact craters vertical plane containing the track. Arrow length is proportional to tilt.
(arrows) within and in the vicinity of the Caloris basin superimposed on Dashed line shows the ground track of the profile in (B). (B) Profile
regional topography. Tilts are obtained from representative MLA tracks MLASCIRDR1107292041 across the 100-km-diameter crater Atget dem-
across each crater and constitute the projection of total tilt onto the onstrates northward tilt of the crater floor.
www.sciencemag.org SCIENCE VOL 336 13 APRIL 2012 219
5. REPORTS
topographic model, in contrast, is precisely 3. The MLA is a time-of-flight laser rangefinder that uses direct 19. C. I. Fassett et al., abstr. 142-6, paper presented at the
controlled and enables confident characteriza- detection and pulse-edge timing to determine precisely Geological Society of America annual meeting,
the range from the MESSENGER spacecraft to Mercury’s Minneapolis, 9 to 12 October 2011; http://gsa.confex.
tion of long-wavelength topography. MLA ob- surface. MLA’s laser transmitter emits 5-ns-wide pulses at an com/gsa/2011AM/finalprogram/abstract_196331.htm.
servations confirm that the northern floor of 8-Hz rate with 20 mJ of energy at a wavelength of 1064 20. C. Klimczak et al., abstr. 142-10, paper presented at the
Caloris is elevated relative to other parts of the nm. Return echoes are collected by an array of four Geological Society of America annual meeting,
basin interior, so much so that in places the refractive telescopes and are detected with a single silicon Minneapolis, 9 to 12 October 2011; http://gsa.confex.
avalanche photodiode detector. The timing of laser pulses is com/gsa/2011AM/finalprogram/abstract_195048.htm.
floor lies above the basin rim (Fig. 3). This measured with a set of time-to-digital converters and 21. S. L. Murchie et al., Science 321, 73 (2008).
portion of the floor of Caloris appears to be counters and a crystal oscillator operating at a frequency 22. J. W. Head et al., Space Sci. Rev. 131, 41 (2007).
part of a quasi-linear rise that trends generally that is monitored periodically from Earth. 23. J. Oberst et al., Icarus 209, 230 (2010).
west-southwest–east-northeast and extends 4. D. E. Smith et al., Science 336, xxx (2012); 24. C. I. Fassett, S. J. Kadish, J. W. Head, S. C. Solomon,
10.1126/science.1218809. R. G. Strom, Geophys. Res. Lett. 38, L10202
over approximately half the circumference of 5. M. T. Zuber et al., Science 321, 77 (2008). (2011).
Mercury at mid-latitudes (Fig. 1A). The floors 6. M. T. Zuber, D. E. Smith, F. G. Lemoine, G. A. Neumann, 25. S. D. King, Nat. Geosci. 1, 229 (2008).
of younger impact craters within and near Caloris Science 266, 1839 (1994). 26. N. Michel et al., P41A-1581, paper presented at the
(Fig. 3) display departures from the horizontal 7. D. E. Smith et al., Science 284, 1495 (1999). American Geophysical Union fall meeting, San Francisco,
8. P. D. Spudis, J. E. Guest, in Mercury, F. Vilas, C. R. Chapman, 5 to 9 December 2011.
that generally correlate with regional tilts im-
M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 27. A. J. Dombard, S. A. Hauck II, S. C. Solomon, Lunar
parted by the long-wavelength topography of AZ, 1988), pp. 118–164. Planet. Sci. 32, abstr. 2035 (2001).
the region and are consistent with modifica- 9. S. C. Solomon et al., Science 321, 59 (2008). 28. M. T. Zuber et al., Icarus 209, 247 (2010).
tion of Mercury’s long-wavelength topogra- 29. M. A. Kreslavsky, J. W. Head III, J. Geophys. Res. 105,
Downloaded from www.sciencemag.org on September 21, 2012
10. S. A. Hauck II, S. C. Solomon, D. A. Smith, Geophys. Res.
phy some time after the formation of Caloris Lett. 34, L18201 (2007). 26695 (2000).
11. S. Zhong, M. T. Zuber, J. Geophys. Res. 105, 4153 (2000).
and the emplacement of its interior and ex- 12. See supplementary materials on Science Online. Acknowledgments: The MESSENGER project is supported by
terior volcanic plains. 13. D. E. Smith et al., Icarus 209, 88 (2010). the NASA Discovery Program under contracts NAS5-97271
The changes in long-wavelength topogra- 14. P. Goldreich, A. Toomre, J. Geophys. Res. 74, 2555 (1969). to the Johns Hopkins University Applied Physics Laboratory
phy within the Caloris basin and northern plains, 15. Median differential slope (29) removes the effect of and NASW-00002 to the Carnegie Institution of Washington.
larger-scale tilts from the elevation difference at a given We are grateful for the myriad contributions from the
and perhaps elsewhere on Mercury, occurred MLA instrument and MESSENGER spacecraft teams, and we
baseline length. At each location x, half the difference
after both the end of heavy impact bombard- in elevations between points one baseline length ahead appreciate three helpful reviews of an earlier version of the
ment and the emplacement of the largest ex- and one behind along the altimetry ground track is paper.
panses of volcanic plains on the planet. One subtracted from the difference in elevation between points
possible source of long-wavelength topogra- one-half baseline length ahead and one-half behind, as
Supplementary Materials
tan a = {h[x + (l/2)] – h[x – (l/2)] – 0.5[h(x + l) – h(x – l)]}/l,
phy is the isostatic response to variations in where h is elevation, l is the baseline length, and a is
www.sciencemag.org/cgi/content/full/science.1218805/DC1
crustal thickness. However, the oldest terrains Materials and Methods
the differential slope.
Figs. S1 and S2
on Mercury display crater size-frequency dis- 16. J. W. Head et al., Science 333, 1853 (2011).
Table S1
tributions at large crater diameters similar to 17. L. R. Nittler et al., Science 333, 1847 (2011). Reference (30)
those on the most densely cratered parts of the 18. L. R. Nittler et al., abstr. 142-3, paper presented at
the Geological Society of America annual meeting, 6 January 2012; accepted 2 March 2012
Moon (24). Thus, crustal formation substan- Minneapolis, 9 to 12 October 2011; http://gsa.confex. Published online 21 March 2012;
tially predated long-wavelength topographic com/gsa/2011AM/finalprogram/abstract_193666.htm. 10.1126/science.1218805
change and cannot explain the observations. A
second possible source of such long-wavelength
change in topography is mantle convection (25).
However, recent mantle convection simulations ESCRT-III Governs the Aurora
(26) constrained by internal structure models
consistent with Mercury’s long-wavelength grav-
ity field (4) and by the latitudinal distribution of
B–Mediated Abscission Checkpoint
surface insolation do not produce surface de-
formation of the magnitude required to explain
Through CHMP4C
the observed topography. Another contribution
to topographic change is volcanic and magmatic Jeremy G. Carlton,* Anna Caballe, Monica Agromayor, Magdalena Kloc, Juan Martin-Serrano†
loading of the lithosphere along with its flexural
response, which has a predictable pattern. Fi- The endosomal sorting complex required for transport (ESCRT) machinery plays an evolutionarily
nally, long-wavelength changes in topography conserved role in cytokinetic abscission, the final step of cell division where daughter cells are
could be a deformational response to interior physically separated. Here, we show that charged multivesicular body (MVB) protein 4C (CHMP4C),
planetary cooling and contraction (27). Evidence a human ESCRT-III subunit, is involved in abscission timing. This function correlated with its
for topographic changes during Mercury’s evo- differential spatiotemporal distribution during late stages of cytokinesis. Accordingly, CHMP4C
lution is consistent with evidence from the geom- functioned in the Aurora B–dependent abscission checkpoint to prevent both premature resolution
etry of ridges and lobate scarps that these features of intercellular chromosome bridges and accumulation of DNA damage. CHMP4C engaged the
accommodated surface strain over a substan- chromosomal passenger complex (CPC) via interaction with Borealin, which suggested a model
tial fraction of Mercury’s geological history whereby CHMP4C inhibits abscission upon phosphorylation by Aurora B. Thus, the ESCRT
(28). Observations of the topography add to machinery may protect against genetic damage by coordinating midbody resolution with the
the growing body of evidence that Mercury abscission checkpoint.
was a tectonically, volcanically, and dynami-
cally active planet for much of its evolution. he final separation of daughter cells during tion (6, 7) and human immunodeficiency virus–
References and Notes
1. J. F. Cavanaugh et al., Space Sci. Rev. 131, 451
(2007).
T cytokinesis is the ancestral function of
the endosomal sorting complex required
for transport (ESCRT) machinery (1–5) which
1 (HIV-1) budding (8, 9). Midbody recruitment
of ESCRT-III, the filament-forming scission ma-
chinery, is an essential event in cytokinesis that is
2. S. C. Solomon, R. L. McNutt Jr., R. E. Gold, D. L. Domingue, also acts to resolve equivalent membrane scission thought to provide constrictive force during ab-
Space Sci. Rev. 131, 3 (2007). events in multivesicular body (MVB) forma- scission (2, 10–12). An Aurora B–dependent
220 13 APRIL 2012 VOL 336 SCIENCE www.sciencemag.org