Source: https://www.hou.usra.edu/meetings/lpsc2019/pdf/lpsc2019_program.htm
Timestamp: 2019-04-21 22:45:12+00:00

Document:
Monday Morning, March 18, 8:30 a.m.
Monday Afternoon, March 18, 1:30 p.m.
Monday Afternoon, March 18, 2:30 p.m.
Habitability: Too Hot! Too Cold! Ah, Just Right!
Monday Evening, March 18, 5:30 p.m.
Tuesday Morning, March 19, 8:30 a.m.
Tuesday Morning, March 19, 10:15 a.m.
Tuesday Afternoon, March 19, 1:30 p.m.
Tuesday Afternoon, March 19, 3:15 p.m.
Wednesday Morning, March 20, 8:30 a.m.
Wednesday Morning, March 20, 10:15 a.m.
Wednesday Afternoon, March 20, 1:30 p.m.
Astrobiology: I Saw the Sign… of Life?
Thursday Morning, March 21, 8:30 a.m.
From Meteorites to Asteroids and Back Again!
Thursday Afternoon, March 21, 1:30 p.m.
Thursday Afternoon, March 21, 3:15 p.m.
Friday Morning, March 22, 8:30 a.m.
Tuesday Evening, March 19, 6:00 p.m.
Thursday Evening, March 21, 6:00 p.m.
Poster Session II: Astrobiology Missions and Instrumentation: Boldly Going Where No Spectrometer has Gone Before!
Bjonnes E. * Johnson B. C. Andrews-Hanna J. C.
We simulate basin formation on the Moon to better understand the surface and interior conditions that affect formation.
Jackson A. P. * Perera V. Elkins-Tanton L. T. Asphaug E.
Impacts puncture crust / Exposing magma to space / But of what size and shape?
Trowbridge A. J. * Johnson B. C. Freed A. M. Melosh H. J. Graves K.
Modeling the full evolution of South-Pole Aiken basin to understand the different formation mechanics between mid-sized and large lunar basins.
White L. F. * Cernok A. Darling J. R. Whitehouse M. Joy K. H. et al.
A 4.33 Ga baddeleyite in lunar troctolite 76535 records phase heritage of a high temperature (>2300 C) cubic-ZrO2 precursor suggestive of origin in impact melt.
Gleißner P. * Becker H.
New data on highly siderophile element abundances in lunar impactites will be discussed with respect to their crustal provenance and inferred time of formation.
Moriarty D. P. III * Watkins R. N. Valencia S. N. Kendall J. D. Petro N. E.
Integrating remote sensing datasets, we evaluate the composition and geology of Th-enhanced materials within SPA. Conclusion: Exposure of stratified mantle.
Venkatadri T. K. * Petro N. E.
We modeled ejecta composition in the Crisium and Nectaris Basins to select possible future landing sites with abundant surface material from both basins.
Poehler C. M. * Hiesinger H. van der Bogert C. H.
We determined the absoulte model ages for light plains in the lunar northern region and studied their implications for the origin of light plains.
Speyerer E. J. * Povilaitis R. Z. Robinson M. S. Martin A. C. Boyd A. et al.
Newly formed impacts discovered with LROC images provide new insight into the cratering process and the rate regolith matures on the surface of the Moon.
Wang J. T. * Kreslavsky M. A. Liu J. Z. Head J. W. Kolenkina M. M.
Topographic roughness and thermophysical properties of subunits of impact craters give insight into crater degradation and aid stratigraphic age estimation.
Allen C. C. * Costello E. S. Hayne P. O. Paige D. A.
The gardening rate calculated from km-scale streaks on the Aristarchus plateau is closely comparable to rates estimated from impact modeling and Apollo cores.
Hahn T. M. Jr. * Watkins R. N. Schonwald A. R. Martin A. C. Robinson M. S. et al.
We examine outstanding Apollo 17 science questions through photometric investigation of the TLV using Apollo 17 soils and the Apollo 16 LISCT as ground-truth.
Garvin J. B. * Jones J. S. Sietins J. M. Kent R. Green W. H. et al.
High resolution X-ray computed tomography of Apollo 16 samples reveals the topology and interior deformation of micro-craters at micron-scales.
Semprich J. * Treiman A. H. Filiberto J. Schwenzer S. P.
Phase equilibria modeling is used to calculate low-grade metamorphic phases for likely martian compositions as a function of variations in fluid composition.
Ott J. P. * Rampe E. B. Morris R. V. Treiman A. H.
Sanidine on Mars / The question: how did it form? / Unit cells tell more.
Nekvasil H. * DiFrancesco N. D. Rogers A. D. King P. L.
Martian dust likely contains significant amounts of magmatic gas condensates (halides, oxides, sulfides) and secondary reaction products involving these phases.
Rogaski A. * Ustunisik G. K. Yang S. Humayun M.
Experimental determination of the behavior of Ge, Zn, and Li in the presence of various volatile loads and the associated alteration due to fumarolic degassing.
Yang S. * Humayun M. Righter K. Peslier A. H. Zanda B. et al.
LA-ICP-MS analyses of two ancient shergottites (NWA 7635 and NWA 8159) show a 2Ga year history of germanium degassing from shergottites.
Payre V. * Siebach K. L. Dasgupta R. Rampe E. B.
The chemistry of primary and detrital igneous minerals in Gale Crater, Mars, can be explained by fractional crystallization of shallow hydrated crustal melts.
Phillips M. S. * Viviano C. E. Moersch J. E.
Ancient Hellas rocks / Reveal plagioclase in / Reflectance spectra.
Liebske C. * Khan A.
We statistically mix chondritic and achondritic meteorties to reconcile geochemical signatures, geophysical properties, and redox characteristics of Mars.
Griffin S. * Daly L. Lee M. R. Piazolo S. Trimby P. W. et al.
Large Area Electron Backscatter Diffraction (EBSD) has been applied to ten nakhlites to investigate their slip systems.
Paquet M. * Day J. M. D. Udry A. Hattingh R. Kumler B. et al.
Highly siderophile element abundances in shergottite sulfides seem to be controlled by petrogenetic processes such as fractional crystallization.
Oxygen fugit / Once molten rock travels space / Mars secrets revealed.
Rahib R. R. Udry A. * Howarth G. H. Paquet M. Combs L. M. et al.
Enriched and intermediate poikilitic shergottites have similar emplacement histories but were likely emplaced in different shallow sills in the martian crust.
Balta J. B. * Castle N. Ennis M. E. McSween H. Y.
Oxygen rises / Deep in martian olivine / Tiny chromites form.
Stern S. A. * Spencer J. R. Weaver H. A. Olkin C. B. Moore J. M. et al.
On 1 Jan 2019, NASA’s New Horizons mission conducted a close flyby of KBO 2014 MU69 nicknamed Ultima Thule. Here we summarize the earliest results of that flyby.
Moore J. M. * McKinnon W. B. Spencer J. R. Stern S. A. Binzel R. P. et al.
Overview of very preliminary limited-data geological analysis of MU69, with the promise that many new, quite substantial results will be presented at the talk.
Grundy W. M. * Binzel R. P. Britt D. T. Buie M. W. Cook J. C. et al.
McKinnon W. B. * Stern S. A. Weaver H. A. Spencer J. R. Buie M. W. et al.
MU69’s contact binary shape provides the clearest view to date of the accretion processes operative in the protosolar nebula and subsequent planetesimal disk.
Buie M. W. * Porter S. B. Tamblyn P. Terrell D. Verbiscer A. J. et al.
Four occultations were observed by 2014MU69 and the results were invaluable for mission planning and execution of the New Horizons flyby on 2019 Jan 1.
Porter S. B. * Bierson C. J. Umurhan O. Beyer R. A. Lauer T. A. et al.
Two siblings hold hands / Spinning together in the void / Now visited.
Schenk P. * Beyer R. Beddingfield C. Bierson C. J. Moore J. M. et al.
Bi-lobed orb that rules the night / Ultima Thule is out of sight / Small-scale topography will shed some light.
Zangari A. M. * Beddingfield C. B. Benecchi S. D. Beyer R. A. Bierson C. J. et al.
Why no one found a / Rotation period / On spacecraft approach.
Howett C. J. A. * Parker A. H. Olkin C. B. Protopapa S. Grundy W. et al.
First results of 486958 MU69 are presented; it is shown to be red and bi-lobed. The two lobes have a consistent color, while the neck region is less red.
Spencer J. R. * Showalter M. R. Lauer T. R. Buie M. W. Porter S. B. et al.
New Horizons conducted extensive searches for rings and moons during its flyby of 2014 MU69. As of the time of writing, none have been found.
Weaver H. A. * Stern S. A. Britt D. T. Buratti B. J. Cheng A. F. et al.
MU69 vs. Cometary Nuclei: Comparisons of shapes and surfaces.
Protopapa S. * Grundy W. M. Olkin C. B. Howett C. J. A. Parker A. H. et al.
We compare the composition of 2014MU69 with that of comets to determine which features of comets are primitive and which have emerged because of their history.
Singer K. N. * McKinnon W. B. Spencer J. R. Weaver H. A. Lauer T. R. et al.
The craters on 2014 MU69, or the lack thereof, will provide information on the evolution of the body itself and the size-distribution of Kuiper belt objects.
Jin Z. L. * Bose M.
Orthopyroxenes from four ordinary chondrites have been measured for hydrogen isotope compositions and water contents using SIMS instruments.
Shimizu K. * Alexander C. M. O’D. Hauri E. H. Sarafian A. R. Jacobsen S. D. et al.
Heavier H isotopic composition of mesostases in ordinary chondrites than in carbonaceous chondrites due to inheritance from D-rich ice or Fe oxidation by water.
Greenwood R. C. * Howard K. T. King A. J. Lee M. R. Burbine T. H. et al.
CM chondrites may originate from a diverse range of asteroids or alternatively the CM parent body was more isotopically heterogeneous than previously considered.
Vacher L. G. * Piralla M. Piani L. Marrocchi Y.
We analyzed in situ O-isotopic compositions on calcite in the CM Murchison and Mukundpura in order to track the evolution temperature of CM parent body(ies).
Donohue P. H. * Huss G. R. Nagashima K.
New synthetic manganese- and chromium-bearing carbonate standards allow us to re-investigate Mn-Cr systematics of carbonates in CM chondrites.
Higashi K. * Mikouchi T. Zolensky M. E.
We studied aqueously altered E chondrite clasts in Kaidun and found two types of altered materials and elongate calcite, suggesting separate alteration events.
Abreu N. M. * Corrigan C. M. Keller L. P. Hezel D. C. Gross J. et al.
CR mesostases have primary crystalline nanophases, compositional differences between chondrules setting, and lack trends attributable to elemental mobilization.
Brearley A. J. * Simon S. B.
TEM studies of a chromite-bearing vein in a ferroan olivine phenocryst in a type IIA chondrule in Kainsaz contain compositionally-zoned grains.
Hellmann J. L. * Kruijer T. S. Van Orman J. A. Metzler K. Kleine T.
Cooling rates and cooling ages of ordinary chondrites inversely correlate, indicating that the onion shell structure of their parent bodies was largely retained.
Li Y. * Rubin A. E. Hsu W. Ziegler K.
The twice-shocked NWA 11004 OC has 4-mm poikilitic opx (as in acapulcoites but not type-6 OC); this indicates very high temp. At 4546 Ma, it cooled at <5°C/Ma.
Nakanishi N. * Yokoyama T. Okabayashi S. Iwamori H.
We discuss the thermal history of metal phases to understand physicochemical conditions in the early outer solar system where Isheyevo parent body has formed.
Lunning N. G. * McCoy T. J. Schrader D. L. Nagashima K. Corrigan C. M. et al.
These sulfide-rich iron meteorites provide evidence of much larger scale impact melting on carbonaceous chondrite asteroids than previously recognized.
Anzures B. A. * Parman S. W. Boesenberg J. S. Milliken R. E.
Reduced meteorites and experiments have trace S, H, C, and F in enstatite. Assuming saturation, S and C can be used to estimate fO2 and volatile content of melt.
Heslar M. F. * Barnes J. W. Dhingra R. D. Sotin C. Soderblom J. M.
We discover consistent wave motion in Bayta Fretum, a narrow channel in Kraken Mare, in a dedicated survey of the T100-T126 flybys.
Poggiali V. P. * Mastrogiuseppe M. M. Hayes A. G. H.
We present the bathymetry obtained from the analysis of radar altimeter data acquired during flyby T104 of Titan, during which Cassini observed the Kraken mare.
Farnsworth K. * Chevrier V. Czaplinski E. Soderblom J. M.
This study experimentally explores the liquids viable to freezing on Titan’s surface by investigating the solidus curve of methane-ethane-nitrogen mixtures.
Hanley J. * Groven J. J. Grundy W. M. Dustrud S. Engle A. E. et al.
Two liquid layers / Exist at depth in the seas / Of the moon Titan.
Dhingra R. D. * Barnes J. W. Hedman M. H. Radebaugh J.
We use ‘form follows process’ to quantify shapes of Titan’s lakes to hash out the probable formation scenarios.
Czaplinski E. C. * Farnsworth K. K. Chevrier V. F.
Updated chamber / Gives new insights to Titan’s / Evaporation.
Cable M. L. * Vu T. H. Maynard-Casely H. E. Hodyss R.
Around Titan’s lakes / Butane and acetylene / A co-crystal make!
Malaska M. J. * Lopes R. M. C. Hayes A. Schoenfeld A. Verlander T. et al.
Organic airfall / Covering Titan’s surface / How much is down there?
Gregg T. K. P. * Sakimoto S. E. H.
Titan’s methane flows / Eroding and transporting / Sediment slowly.
Matulka P. R. * Levy J. S. Burr D. M. Maue A. D.
Tumbling clasts of ice / Comminution and rounding / Cryogenic cracks.
Yu X. * Hörst S. M. He C. McGuiggan P.
Organic sand on Titan / Contacting and rubbing / Could it produce electrostatic forces?
Lalich D. E. * Hayes A. G.
Newly processed Cassini RADAR altimetry enables a fresh perspective on Titan’s mountainous terrain.
MacKenzie S. M. * Lorenz R. D. Lora J. M.
Some places heat fast / Some places heat slow — we think. / Dry atmo cares not.
Costello E. S. * Ghent R. R. Lucey P. G.
Moon and Mercury / Icy poles so different / Broken by impacts.
Kulchitsky A. V. * Hurley D. M. Johnson J. B.
Study presents a model of water migration on meso-scale level to determine macro-scale mass transfer rates of water through regolith under different conditions.
Patterson G. W. * Petro N. Keller J. Mandt K. E. McClanahan T. et al.
As LRO looks toward its next extended mission, the polar craters Cabeus and Amundsen stand out for their potential to address key lunar exploration questions.
Luchsinger K. M. * Chanover N. J. Strycker P. D.
We present an analysis of a family of permanently shadowed lunar sediment models, including water ice content, fit to the LCROSS ground-based observations.
Williams J.-P. * Greenhagen B. T. Paige D. A. Schorghofer N. Aye K.-M. et al.
Seasonal temperature mapping of the south pole using LRO Diviner shows the amount of water cold-trapping area more than doubles between summer and winter.
Kloos J. L. * Moores J. E. Sangha J. Nguyen T. G. Schorghofer N.
We explore the influence of seasonal changes in cold trapping area on water transport, trapping and distribution within PSRs at the north and south pole.
Wilson J. T. * Lawrence D. J. Miller R. S. Garrick-Bethell I. Siegler M. A.
Via image reconstruction, we improved the resolution of the LP neutron data to better estimate the hydrogen abundance in areas hypothesized to contain excess H.
Hayne P. O. * Siegler M. A. Paige D. A. Lucey P. G. Fisher E. A.
Shadows in shadows / Collecting comet samples / Why don’t we go see?
Colaprete A. * Elphic R. C. Shirley M.
This paper provides an analysis of the number and distribution of observations needed to provide the necessary next steps in lunar volatile exploration.
Banerdt W. B. * Smrekar S. Antonangeli D. Asmar S. Banfield D. et al.
Status and summary of early results from the InSight mission: Trust my crystal ball? / Instruments remain healthy / Geophysics reigns!
Golombek M. * Warner N. H. Grant J. Hauber E. Ansan V. et al.
InSight landed on a smooth, flat pebble rich surface with low rock abundance, impact craters in various stages of degradation, and eolian bed forms.
Lognonné P. * Banerdt W. B. Pike W. T. Giardini D. Banfield D. et al.
This provides first scientific observations of SEIS for Mars micro-seismic noise, atmospheric-generated signals, and surface and subsurface elastic structure.
Pike W. T. * Lognonne P. Banerdt W. B. Calcutt S. B. Standley I. M. et al.
The dynamic environment at the InSight landing site has been observed with its short-period seismometers.
Spohn T. * Grott M. Smrekar S. E. Knollenberg J. Hudson T. L. et al.
The Heat Flow and Physical Properties Package on InSight is planned to measure the geothermal heat flow of Mars. First results after landing will be presented.
Banfield D. * Spiga A. Newman C. Lorenz R. Forget F. et al.
InSight sees weather / ‘Round the clock and precisely / First results discussed.
Newman C. E. * Viudez-Moreiras D. Baker M. M. Lewis K. W. Gomez-Elvira J. et al.
Comparing atmospheric model predictions for the InSight/MSL region with observed wind and aeolian features improves understanding of the key physical processes.
Miljkovic K. * Collins G. S. Rajsic A. Wojcicka N. Neidhart T. et al.
Simulations of meteoroid strikes on Mars using iSALE-2D code and connecting impact and target properties with properties of seismic waves generated by impacts.
Plesa A.-C. * Padovan S. Tosi N. Breuer D. Grott M. et al.
We present how thermal evolution models of interior dynamics of Mars can be improved by the measurements of the InSight mission.
Showalter M. R. * Buie M. W. Grundy W. M. Hamilton D. P. Kaufmann D. E. et al.
The hypothesis that many KBOs are contact binaries (similar in shape to 2014 MU69) has testable implications for the distribution of KBO lightcurves.
Verbiscer A. J. * Porter S. B. Benecchi S. D. Kavelaars J. J. Weaver H. A. et al.
Kuiper belt objects / Scatter feeble sunlight to / Show surface texture.
Beyer R. A. * Weaver H. A. Porter S. B. Grundy W. M. Moore J. M. et al.
These are the New Horizons Team’s initial thoughts about how to apply mapping schemes and cartographic reference systems to the bi-lobate contact binary MU69.
Keane J. T. * Bierson C. J. Lisse C. M. Showalter M. W. Stansberry J. A. et al.
MU69 / Little gravity, steep slopes / Good skiing at neck.
Lisse C. M. * Singer K. N. Fernandez Y. R. Bauer J. M. Protopapa S. et al.
Spitzer/WISE JF comet and new NH Pluto/Charon KBO size-frequency distributions are similar; another piece of evidence that the populations are genetically linked.
Pluto and other dwarf planets can influence the stability of Classical Kuiper Belt objects causing them to be short period comets.
Hofgartner J. D. * Buratti B. J. Hayne P. O. Young L. A.
Eris is anomalously bright; it is likely active. We test the hypothesis of atmospheric collapse for its albedo with a numerical model and find that it is unlikely.
Poppe A. R. * Horányi M.
We use an interplanetary dust dynamics model and a dust ablation model to calculate the deposition of water at Pluto and Triton’s atmospheres from dust.
Buratti B. J. * Hicks M. D. Kramer E. Bauer J.
We report on observations of Pluto and Charon when they are fully illuminated, a geometry that will not be repeated for 161 years. Both are anomalously bright.
Mills F. P. * Marcq E. Yung Y. Parkinson C. D. Jessup K. L. et al.
This presentation discusses the current understanding of atmospheric chemistry on Venus and key outstanding issues.
Korablev O. Montmessin F. * Fedorova A. Trokhimovskiy A. Ignatiev N. et al.
Latest results from the ACS instrument onboard TGO over the period from the Science Phase start (04/2018) until the end of the 2018 dust event will be presented.
Kite E. S. * Steele L. J. Mischna M. A.
A cold-start H2O(i) cloud greenhouse can sustain T > 290K on early Mars for >>100yr in equilibrium with polar/mountain-top ice, but only if the planet is arid.
Warren A. O. * Kite E. S.
We present a new martain paleopressure estimate before 4 Ga and use this alongside existing constraints in a basic 2-component Mars atmosphere evolution model.
Smith C. L. * Moores J. E. Guzewich S. D. Ellison D.
Global dust storm caused / Low visibility for / Curiosity.
Corlies P. * Hayes A. G. Kelland J. Adamkovics M. Rodriguez S. et al.
We present an update on ongoing monitoring of clouds on Titan, as well as an analysis of Titan’s clouds, including wind profiles of Titan’s atmosphere.
Kutsop N. W. * Hayes A. G. Sotin C. Lunine J. L. Corlies P. M. et al.
We report the detection of annular atmospheric features encircling Titan using observation from the Cassini-Huygens Visual and Infrared Mapping Spectrometer.
Jackson B. * Adams E. R. Sandidge W. Kreyche S. Briggs J.
Exo-Jupiters / Searing and turbulent worlds / Clouds whorl violently.
Kohler E. * Ferguson F. Marcum S.
Experiments were conducted to directly measure the evaporation rate of fosterite for use in exoplanet cloud formation models.
We estimate that there are at least five major types of habitable worlds. Those more abundant are harder to detect and those similar to Earth are less common.
Abramov O. * Brasser R. Mojzsis S. J.
This presentation will outline our current understanding of late accretion impact bombardment and discuss its thermal, geochemical, and biological effects.
Moore C. A. * Smith C. L. Moores J. E.
A theoretical exercise to assess the depth into the subsurface at which terrestrial radioresistant organisms can survive under martian insolation.
Chevrier V. F. * Rivera-Valentín E. G. Soto A. Altheide T. S. Melchiorri R.
Deliquescence of brines only occurs for lowest eutectic salts and at high latitudes on Mars, putting strong limitations on the possibility of special regions.
Stamenkovic V. * Ward L. M. Mischna M. Fischer W. W.
We find that brines on Mars could contain enough oxygen for microbes to breathe.
Smith H. D. * Duncan A. G. Schuerger A. C. McKay C. P.
This study looked at the changes in PLFA content in a microbial community within a salt crust exposed to simulated martain conditions.
Craig P. I. * Mickol R. L. Marnocha C. L. Kral T. A.
Methanogens can grow on Mars-relevant clay minerals without supplemental media, suggesting Noachian Mars could potentially have supported microbial life.
Yazdani A. * Nepal S. Chevrier V. F. Kumar P.
In this study we explore the adaptive evolution of bacteria to high concentrations of magnesium sulfate, which is the dominant salt in Jupiter’s moon Europa.
Hesse M. A. * Jordan J. S. Vance S. D. McCarthy C.
The habitability of Europa’s interior ocean depends on the availability of redox gradients. We study oxidant transport by downward percolation of dense brines.
Teodoro L. * Kegerreis J. Estrada P. Cuzzi J. Eke V. et al.
Impact simulations of the Saturn’s icy moons with unprecedented spatial resolution allow us to shed light on the Saturn’s rings age.
Asphaug E. * Emsenhuber A.
We revisit a scenario for the formation of Saturn’s middle-sized moons via giant impact by taking into account the presence of Saturn in the model.
Gyalay S. * Dodds K. H. Nimmo F.
We translate long-wavelength topography into spatial variations of tidal heating via isostasy. This reveals the interiors of Tethys and Mimas.
Wong T. * Hansen U. Wiesehöfer T. Stellmach S. McKinnon W. B.
Europa’s subsurface ocean can be layered by the process of double-diffusive convection, which may affect heat and material transport through the ocean.
Galileo observations of Io’s heat flux suggest that 50–75% of Io’s tidal heating occurs in a shallow asthenosphere.
Klimczak C. * Byrne P. K. Regensburger P. V. Bohnenstiehl D. R. Hauck, II S. A. et al.
Lots of water makes / The floor strong and hard to break / So not much happens.
Miller K. E. * Glein C. R. Waite J. H. Bolton S. J.
Water, organics / H exchange in heated cores / Varies in extent.
McEwen A. S. * Schafer E. Sutton S. Chojnacki M.
We gonna rock down to electric RSL and then we’ll take it higher.
Tebolt M. * Schorghofer N. Goudge T. Levy J.
We examine the possibility of various wet and dry formation processes of recurring slope lineae by analyzing the physical characteristics of 10,000+ RSL.
Heyer T. * Kreslavsky M. Hiesinger H. Reiss D. Bernhardt H. et al.
Seasonal variations in slope streak activity were observed at intermediate latitudes as well as at the equator.
Imamura S. * Sekine Y. Maekawa Y. Sasaki T.
Results of laboratory experiments suggest that due to salt precipitation within soils, brine flow forms elongated streaks on Mars even at a low flow rate.
Guimpier A. * Conway S. J. Mangeney A. Peruzzetto M. Mangold N.
Report on a landslide near the Nili Fossae region on Mars whose morphology resembles mudslides on Earth.
Raack J. * Conway S. J. Heyer T. Philippe M. Hiesinger H. et al.
Study of present-day active gullies in Sisyphi Cavi: Exact timings, thermal investigations, orientations, and presentation of a potential formation mechanism.
Khuller A. R. * Christensen P. R.
We present novel visible, spectral, and thermal evidence of decameter-scale, water-rich snow deposits being exhumed within mid-latitude gully alcoves.
Parsons R. A. * Hemmi R. Miyamoto H. Kanzaki T.
Obliquity-induced temperature variations influence the flow rate of an advancing equatorial ice sheet — facilitating ridge deposition on Tharsis Montes flanks.
Soare R. J. * Conway S. J. Williams J.-P. Gallagher C. Mc Keown L. E.
We discuss martian mounds, whose shape, traits, scale, and spatially-associated landscape features would be expected were the mounds closed-system pingos.
Grimm R. E. * Michaels T. Stillman D. E.
RSL at five sites can initiate as liquid flows with the same ice-melting temperature near 250 K by considering differences in shallow subsurface structure.
Knightly J. P. * Fusco M. S. Farnsworth K. Chevrier V. F.
Observations of temporal variations and potential factors influencing the growth rate of Swiss Cheese Terrain on the south polar cap between Mars years 28–34.
Hao J. * Michael G. G. Adeli S. Hauber E. Portyankina G. et al.
Regional variation in the spiders’ local spatial distribution was discussed. We tried to investigate possible constraints on spider spatial patterns.
Mc Keown L. E. * Bourke M. C. McElwaine J. N. Sylvest M. E. Patel M. R.
We present the first laboratory observations of the formation of araneiforms by CO2 sublimation and the results of a survey of araneiform morphometry on Mars.
Lauretta D. S. * Al Asad M. M. Ballouz R. L. Barnouin O. S. Bierhaus E. B. et al.
We report the initial assessment of asteroid Bennu from data acquired during the Approach and Preliminary Survey phases of the OSIRIS-REx mission.
Barnouin O. S. * Palmer E. Gaskell B. Weirich J. Daly M. et al.
We present results on the shape of Bennu, using newly acquired data by the OSIRIS-REx mission.
Susorney H. C. M. * Johnson C. L. Barnouin O. S. Daly M. G. Al Asad M. M. et al.
Shape model studied / Surface roughness of Bennu / Boulders and craters.
Al Asad M. M. * Johnson C. L. Barnoiun O. S. Daly M. Palmer E. et al.
We present a summary of our efforts for assessing and evaluating the shape models produced by stereophotoclinometric (SPC) models of asteroid Bennu.
Scheeres D. J. * McMahon J. W. French A. S. Brack D. N. Leonard J. et al.
The global geophysical implications and interpretations of Bennu’s estimated mass, shape, and spin state are discussed.
Rizk B. * DellaGiustina D. N. Golish D. R. Bennett C. A. Drouet d’Aubigny C. et al.
The OSIRIS-REx Camera Suite (OCAMS) PolyCam and MapCam early images of Bennu reveal a fascinating small body.
Walsh K. J. * Jawin E. R. McCoy T. Connolly H. C. Jr. Lauretta D. S. et al.
A global overview of the geology of NEA Bennu, including its craters, boulders, linear features, and regolith.
Ballouz R.-L. * Walsh K. J. Schwartz S. R. Baresi N. Barnouin O. S. et al.
Impacts and spin-up / Move grains on Bennu’s surface / Craters disappear.
Jawin E. R. * Walsh K. J. Barnouin O. S. McCoy T. J. Ballouz R.-L. et al.
The largest boulders on Bennu are diverse in their apparent lithology and local geologic setting.
Molaro J. L. * Delbo M. Ballouz R.-L. Jawin E. Walsh K. et al.
We relate numerical simulations to observations to explore the role that thermally induced stresses play in the development of fractures on Bennu’s surface.
Emery J. P. * Rozitis B. Christensen P. R. Hamilton V. E. Simon A. A. et al.
Full-disk thermal observations of Bennu from OSIRIS-REx are analyzed to derive thermophysical properties of Bennu’s surface.
Hamilton V. E. * Simon A. A. Christensen P. R. Reuter D. C. Della Giustina D. N. et al.
VNIR and TIR spectrometers onboard OSIRIS-REx have revealed evidence of hydrated phases across the surface of asteroid (101955) Bennu.
Simon A. A. * Reuter D. C. Howell E. S. Clark B. E. Hamilton V. E. et al.
Hello, small Bennu! / Hydration seen everywhere / What secrets await?
Anderson R. C. * Dohm J. M. Siwabessy A. Schroeder J. F.
A detailed reconstruction of the tectonic history of the Memnonia-Sirenum region of Mars is presented here through a new 1:5,000,000-scale USGS map.
Citron R. I. * Manga M.
We examine if following a giant impact on early Mars, a superplume could develop in the hemisphere opposite the impact.
Broquet A. * Wieczorek M. A. Fa W.
Inversion of the present-day geodynamic state of Mars beneath the northern polar cap using elevation data from MOLA and radar data from MARSIS.
Brennan M. C. * Fischer R. A. Irving J. C.
We modeled core formation and planetary structure to explore the parameters of importance for Mars’ core size and the siesmic properties observable by InSight.
Schmerr N. C. * Kawamura T. Margerin L. van Driel M. Garcia R. et al.
Waves grow weak in Mars / What mechanisms drive this loss? / InSight will tell us!
The topography of wrinkle ridges on Mars was analyzed, yielding three main ridge classes. Inversions of the profiles reveal the underlying geometry of faults.
Clark J. D. * van der Bogert C. H. Hiesinger H. Watters T. R. Robinson M. S.
Age determinations for wrinkle ridge-lobate scarp transisitions reveal seismically induced resurfacing by fault slip events in the last 100 Ma.
Martin E. S. * Watters T. R.
We evaluate two mechanisms for producing basin-centric graben on the Moon: (1) Extension due to lithospheric flexure, or (2) shallow-dike-induced dilation.
Yu S. * Tosi N. Schulz F. Schwinger S. Breuer D. et al.
We check the rheological conditions needed for lunar magma ocean overturn in the context of non-linear mantle rheology.

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