# pub2018.bib

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@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c year=2018 -c $type="ARTICLE" -oc pub2018.txt -ob pub2018.bib lmdplaneto.link.bib}}  @article{2018NatGe..11..888W, author = {{Wordsworth}, R. and {Ehlmann}, B. and {Forget}, F. and {Haberle}, R. and {Head}, J. and {Kerber}, L.}, title = {{Healthy debate on early Mars}}, journal = {Nature Geoscience}, year = 2018, volume = 11, pages = {888-888}, doi = {10.1038/s41561-018-0267-5}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018NatGe..11..888W}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123.3020S, author = {{S{\'a}nchez-Lavega}, A. and {Garro}, A. and {del R{\'{\i}}o-Gaztelurrutia}, T. and {Hueso}, R. and {Ordo{\~n}ez-Etxeberria}, I. and {Chen Chen}, H. and {Cardes{\'{\i}}n-Moinelo}, A. and {Titov}, D. and {Wood}, S. and {Almeida}, M. and {Spiga}, A. and {Forget}, F. and {M{\"a}{\"a}tt{\"a}nen}, A. and {Hoffmann}, H. and {Gondet}, B.}, title = {{A Seasonally Recurrent Annular Cyclone in Mars Northern Latitudes and Observations of a Companion Vortex}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {Mars atmosphere, atmospheric dynamics}, year = 2018, volume = 123, pages = {3020-3034}, abstract = {{We study a seasonally recurrent cyclone and related cloud phenomena observed on Mars at L$_{s}$120{\deg}, latitude 60{\deg}N, and longitude 90{\deg}W from images obtained with cameras in different spacecraft between 1995 and 2018. A remarkable double cyclone formed in 2012 and we present a detailed study of its dynamics using images from Mars Express and Mars Reconnaissance Orbiter obtained between 6 June and 9 July. A double cyclone was also observed in 2006 and 2008. In other Martian years the primary cyclone showed an annular cloud morphology with a large water ice cloud observed eastward of it. The cyclones have a size of 600-800 km with a cloud-free core of a radius 100-300 km. Tangential velocities measured from cloud tracking in 2012 images are 5-20 m/s$^{-1}$at 10-km altitude and double cyclone moved eastward with a velocity of 4 m/s$^{-1}$during its lifetime of increasing insolation as the sol progresses, a part of the clouds evaporate, the winds weaken, and the vortices lose coherence. This phenomenon forms under high-temperature gradients in a region with a large north-south topographic slope and has been recurrent each Martian year between 1995 and 2018. We argue the interest of studying its changing properties each Martian year in order to explore their possible relationship to the state of the Martian atmosphere at L$_{s}$120{\deg}. }}, doi = {10.1029/2018JE005740}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123.3020S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..314..232G, author = {{Grundy}, W.~M. and {Bertrand}, T. and {Binzel}, R.~P. and {Buie}, M.~W. and {Buratti}, B.~J. and {Cheng}, A.~F. and {Cook}, J.~C. and {Cruikshank}, D.~P. and {Devins}, S.~L. and {Dalle Ore}, C.~M. and {Earle}, A.~M. and {Ennico}, K. and {Forget}, F. and {Gao}, P. and {Gladstone}, G.~R. and {Howett}, C.~J.~A. and {Jennings}, D.~E. and {Kammer}, J.~A. and {Lauer}, T.~R. and {Linscott}, I.~R. and {Lisse}, C.~M. and {Lunsford}, A.~W. and {McKinnon}, W.~B. and {Olkin}, C.~B. and {Parker}, A.~H. and {Protopapa}, S. and {Quirico}, E. and {Reuter}, D.~C. and {Schmitt}, B. and {Singer}, K.~N. and {Spencer}, J.~A. and {Stern}, S.~A. and {Strobel}, D.~F. and {Summers}, M.~E. and {Weaver}, H.~A. and {Weigle}, G.~E. and {Wong}, M.~L. and {Young}, E.~F. and {Young}, L.~A. and {Zhang}, X.}, title = {{Pluto's haze as a surface material}}, journal = {\icarus}, archiveprefix = {arXiv}, eprint = {1903.03728}, primaryclass = {astro-ph.EP}, keywords = {Pluto, surface, atmosphere, Geological processes, Ices, Photochemistry}, year = 2018, volume = 314, pages = {232-245}, abstract = {{Pluto's atmospheric haze settles out rapidly compared with geological timescales. It needs to be accounted for as a surface material, distinct from Pluto's icy bedrock and from the volatile ices that migrate via sublimation and condensation on seasonal timescales. This paper explores how a steady supply of atmospheric haze might affect three distinct provinces on Pluto. We pose the question of why they each look so different from one another if the same haze material is settling out onto all of them. Cthulhu is a more ancient region with comparatively little present-day geological activity, where the haze appears to simply accumulate over time. Sputnik Planitia is a very active region where glacial convection, as well as sublimation and condensation rapidly refresh the surface, hiding recently deposited haze from view. Lowell Regio is a region of intermediate age featuring very distinct coloration from the rest of Pluto. Using a simple model haze particle as a colorant, we are not able to match the colors in both Lowell Regio and Cthulhu. To account for their distinct colors, we propose that after arrival at Pluto's surface, haze particles may be less inert than might be supposed from the low surface temperatures. They must either interact with local materials and environments to produce distinct products in different regions, or else the supply of haze must be non-uniform in time and/or location, such that different products are delivered to different places. }}, doi = {10.1016/j.icarus.2018.05.019}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..314..232G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..314..149L, author = {{Lebonnois}, S. and {Schubert}, G. and {Forget}, F. and {Spiga}, A. }, title = {{Planetary boundary layer and slope winds on Venus}}, journal = {\icarus}, keywords = {Venus, Atmosphere, Planetary boundary layer, Slope winds}, year = 2018, volume = 314, pages = {149-158}, abstract = {{Few constraints are available to characterize the deep atmosphere of Venus, though this region is crucial to understand the interactions between surface and atmosphere on Venus. Based on simulations performed with the IPSL Venus Global Climate Model, the possible structure and characteristics of Venus' planetary boundary layer (PBL) are investigated. The vertical profile of the potential temperature in the deepest 10 km above the surface and its diurnal variations are controlled by radiative and dynamical processes. The model predicts a diurnal cycle for the PBL activity, with a stable nocturnal PBL while convective activity develops during daytime. The diurnal convective PBL is strongly correlated with surface solar flux and is maximum around noon and in low latitude regions. It typically reaches less than 2 km above the surface, but its vertical extension is much higher over high elevations, and more precisely over the western flanks of elevated terrains. This correlation is explained by the impact of surface winds, which undergo a diurnal cycle with downward katabatic winds at night and upward anabatic winds during the day along the slopes of high-elevation terrains. The convergence of these daytime anabatic winds induces upward vertical winds, that are responsible for the correlation between height of the convective boundary layer and topography. }}, doi = {10.1016/j.icarus.2018.06.006}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..314..149L}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..314....1G, author = {{Garate-Lopez}, I. and {Lebonnois}, S.}, title = {{Latitudinal variation of clouds' structure responsible for Venus' cold collar}}, journal = {\icarus}, keywords = {Venus atmosphere, Cold collar, Modelling}, year = 2018, volume = 314, pages = {1-11}, abstract = {{Global Climate Models (GCM) are very useful tools to study theoretically the general dynamics and specific phenomena in planetary atmospheres. In the case of Venus, several GCMs succeeded in reproducing the atmosphere's superrotation and the global temperature field. However, the highly variable polar temperature and the permanent cold collar present at 60$^{o}$-80$^{o}$latitude have not been reproduced satisfactorily yet. Here we improve the radiative transfer scheme of the Institut Pierre Simon Laplace Venus GCM in order to numerically simulate the polar thermal features in Venus atmosphere. The main difference with the previous model is that we now take into account the latitudinal variation of the cloud structure. Both solar heating rates and infrared cooling rates have been modified to consider the cloud top's altitude decrease toward the poles and the variation in latitude of the different particle modes' abundances. A new structure that closely resembles the observed cold collar appears in the average temperature field at 2 {\times}10$^{4}$- 4 {\times}10$^{3}$Pa ({\sim} 62 - 66 km) altitude range and 60$^{o}$-90$^{o}$latitude band. It is not isolated from the pole as in the observation-based maps, but the obtained temperature values (220 K) are in good agreement with observed values. Temperature polar maps across this region show an inner warm region where the polar vortex is observed, but the obtained 230 K average value is colder than the observed mean value and the simulated horizontal structure does not show the fine-scale features present within the vortex. The comparison with a simulation that does not take into account the latitudinal variation of the cloud structure in the infrared cooling computation, shows that the cloud structure is essential in the cold collar formation. Although our analysis focuses on the improvement of the radiative forcing and the variations it causes in the thermal structure, polar dynamics is definitely affected by this modified environment and a noteworthy upwelling motion is found in the cold collar area. }}, doi = {10.1016/j.icarus.2018.05.011}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..314....1G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018ExA....46..135T, author = {{Tinetti}, G. and {Drossart}, P. and {Eccleston}, P. and {Hartogh}, P. and {Heske}, A. and {Leconte}, J. and {Micela}, G. and {Ollivier}, M. and {Pilbratt}, G. and {Puig}, L. and {Turrini}, D. and {Vandenbussche}, B. and {Wolkenberg}, P. and {Beaulieu}, J.-P. and {Buchave}, L.~A. and {Ferus}, M. and {Griffin}, M. and {Guedel}, M. and {Justtanont}, K. and {Lagage}, P.-O. and {Machado}, P. and {Malaguti}, G. and {Min}, M. and {N{\o}rgaard-Nielsen}, H.~U. and {Rataj}, M. and {Ray}, T. and {Ribas}, I. and {Swain}, M. and {Szabo}, R. and {Werner}, S. and {Barstow}, J. and {Burleigh}, M. and {Cho}, J. and {du Foresto}, V.~C. and {Coustenis}, A. and {Decin}, L. and {Encrenaz}, T. and {Galand}, M. and {Gillon}, M. and {Helled}, R. and {Morales}, J.~C. and {Mu{\~n}oz}, A.~G. and {Moneti}, A. and {Pagano}, I. and {Pascale}, E. and {Piccioni}, G. and {Pinfield}, D. and {Sarkar}, S. and {Selsis}, F. and {Tennyson}, J. and {Triaud}, A. and {Venot}, O. and {Waldmann}, I. and {Waltham}, D. and {Wright}, G. and {Amiaux}, J. and {Auguères}, J.-L. and {Berthé}, M. and {Bezawada}, N. and {Bishop}, G. and {Bowles}, N. and {Coffey}, D. and {Colomé}, J. and {Crook}, M. and {Crouzet}, P.-E. and {Da Peppo}, V. and {Sanz}, I.~E. and {Focardi}, M. and {Frericks}, M. and {Hunt}, T. and {Kohley}, R. and {Middleton}, K. and {Morgante}, G. and {Ottensamer}, R. and {Pace}, E. and {Pearson}, C. and {Stamper}, R. and {Symonds}, K. and {Rengel}, M. and {Renotte}, E. and {Ade}, P. and {Affer}, L. and {Alard}, C. and {Allard}, N. and {Altieri}, F. and {André}, Y. and {Arena}, C. and {Argyriou}, I. and {Aylward}, A. and {Baccani}, C. and {Bakos}, G. and {Banaszkiewicz}, M. and {Barlow}, M. and {Batista}, V. and {Bellucci}, G. and {Benatti}, S. and {Bernardi}, P. and {Bézard}, B. and {Blecka}, M. and {Bolmont}, E. and {Bonfond}, B. and {Bonito}, R. and {Bonomo}, A.~S. and {Brucato}, J.~R. and {Brun}, A.~S. and {Bryson}, I. and {Bujwan}, W. and {Casewell}, S. and {Charnay}, B. and {Pestellini}, C.~C. and {Chen}, G. and {Ciaravella}, A. and {Claudi}, R. and {Clédassou}, R. and {Damasso}, M. and {Damiano}, M. and {Danielski}, C. and {Deroo}, P. and {Di Giorgio}, A.~M. and {Dominik}, C. and {Doublier}, V. and {Doyle}, S. and {Doyon}, R. and {Drummond}, B. and {Duong}, B. and {Eales}, S. and {Edwards}, B. and {Farina}, M. and {Flaccomio}, E. and {Fletcher}, L. and {Forget}, F. and {Fossey}, S. and {Fr{\"a}nz}, M. and {Fujii}, Y. and {Garc{\'{\i}}a-Piquer}, {\'A}. and {Gear}, W. and {Geoffray}, H. and {Gérard}, J.~C. and {Gesa}, L. and {Gomez}, H. and {Graczyk}, R. and {Griffith}, C. and {Grodent}, D. and {Guarcello}, M.~G. and {Gustin}, J. and {Hamano}, K. and {Hargrave}, P. and {Hello}, Y. and {Heng}, K. and {Herrero}, E. and {Hornstrup}, A. and {Hubert}, B. and {Ida}, S. and {Ikoma}, M. and {Iro}, N. and {Irwin}, P. and {Jarchow}, C. and {Jaubert}, J. and {Jones}, H. and {Julien}, Q. and {Kameda}, S. and {Kerschbaum}, F. and {Kervella}, P. and {Koskinen}, T. and {Krijger}, M. and {Krupp}, N. and {Lafarga}, M. and {Landini}, F. and {Lellouch}, E. and {Leto}, G. and {Luntzer}, A. and {Rank-L{\"u}ftinger}, T. and {Maggio}, A. and {Maldonado}, J. and {Maillard}, J.-P. and {Mall}, U. and {Marquette}, J.-B. and {Mathis}, S. and {Maxted}, P. and {Matsuo}, T. and {Medvedev}, A. and {Miguel}, Y. and {Minier}, V. and {Morello}, G. and {Mura}, A. and {Narita}, N. and {Nascimbeni}, V. and {Nguyen Tong}, N. and {Noce}, V. and {Oliva}, F. and {Palle}, E. and {Palmer}, P. and {Pancrazzi}, M. and {Papageorgiou}, A. and {Parmentier}, V. and {Perger}, M. and {Petralia}, A. and {Pezzuto}, S. and {Pierrehumbert}, R. and {Pillitteri}, I. and {Piotto}, G. and {Pisano}, G. and {Prisinzano}, L. and {Radioti}, A. and {Réess}, J.-M. and {Rezac}, L. and {Rocchetto}, M. and {Rosich}, A. and {Sanna}, N. and {Santerne}, A. and {Savini}, G. and {Scandariato}, G. and {Sicardy}, B. and {Sierra}, C. and {Sindoni}, G. and {Skup}, K. and {Snellen}, I. and {Sobiecki}, M. and {Soret}, L. and {Sozzetti}, A. and {Stiepen}, A. and {Strugarek}, A. and {Taylor}, J. and {Taylor}, W. and {Terenzi}, L. and {Tessenyi}, M. and {Tsiaras}, A. and {Tucker}, C. and {Valencia}, D. and {Vasisht}, G. and {Vazan}, A. and {Vilardell}, F. and {Vinatier}, S. and {Viti}, S. and {Waters}, R. and {Wawer}, P. and {Wawrzaszek}, A. and {Whitworth}, A. and {Yung}, Y.~L. and {Yurchenko}, S.~N. and {Osorio}, M.~R.~Z. and {Zellem}, R. and {Zingales}, T. and {Zwart}, F.}, title = {{A chemical survey of exoplanets with ARIEL}}, journal = {Experimental Astronomy}, keywords = {Exoplanets, Space missions, IR spectroscopy, Molecular signatures}, year = 2018, volume = 46, pages = {135-209}, abstract = {{Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet's birth, and evolution. ARIEL was conceived to observe a large number ( 1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25-7.8 {$\mu$}m spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10-100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H$_{2}$O, CO$_{2}$, CH$_{4}$NH$_{3}$, HCN, H$_{2}$S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed - using conservative estimates of mission performance and a full model of all significant noise sources in the measurement - using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL - in line with the stated mission objectives - will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives. }}, doi = {10.1007/s10686-018-9598-x}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018ExA....46..135T}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018SSRv..214..109S, author = {{Spiga}, A. and {Banfield}, D. and {Teanby}, N.~A. and {Forget}, F. and {Lucas}, A. and {Kenda}, B. and {Rodriguez Manfredi}, J.~A. and {Widmer-Schnidrig}, R. and {Murdoch}, N. and {Lemmon}, M.~T. and {Garcia}, R.~F. and {Martire}, L. and {Karatekin}, {\"O}. and {Le Maistre}, S. and {Van Hove}, B. and {Dehant}, V. and {Lognonné}, P. and {Mueller}, N. and {Lorenz}, R. and {Mimoun}, D. and {Rodriguez}, S. and {Beucler}, {\'E}. and {Daubar}, I. and {Golombek}, M.~P. and {Bertrand}, T. and {Nishikawa}, Y. and {Millour}, E. and {Rolland}, L. and {Brissaud}, Q. and {Kawamura}, T. and {Mocquet}, A. and {Martin}, R. and {Clinton}, J. and {Stutzmann}, {\'E}. and {Spohn}, T. and {Smrekar}, S. and {Banerdt}, W.~B.}, title = {{Atmospheric Science with InSight}}, journal = {\ssr}, keywords = {Mars, InSight, Atmospheric science, Planetary atmospheres}, year = 2018, volume = 214, eid = {109}, pages = {109}, abstract = {{In November 2018, for the first time a dedicated geophysical station, the InSight lander, will be deployed on the surface of Mars. Along with the two main geophysical packages, the Seismic Experiment for Interior Structure (SEIS) and the Heat-Flow and Physical Properties Package (HP$^{3}$), the InSight lander holds a highly sensitive pressure sensor (PS) and the Temperature and Winds for InSight (TWINS) instrument, both of which (along with the InSight FluxGate (IFG) Magnetometer) form the Auxiliary Sensor Payload Suite (APSS). Associated with the RADiometer (RAD) instrument which will measure the surface brightness temperature, and the Instrument Deployment Camera (IDC) which will be used to quantify atmospheric opacity, this will make InSight capable to act as a meteorological station at the surface of Mars. While probing the internal structure of Mars is the primary scientific goal of the mission, atmospheric science remains a key science objective for InSight. InSight has the potential to provide a more continuous and higher-frequency record of pressure, air temperature and winds at the surface of Mars than previous in situ missions. In the paper, key results from multiscale meteorological modeling, from Global Climate Models to Large-Eddy Simulations, are described as a reference for future studies based on the InSight measurements during operations. We summarize the capabilities of InSight for atmospheric observations, from profiling during Entry, Descent and Landing to surface measurements (pressure, temperature, winds, angular momentum), and the plans for how InSight's sensors will be used during operations, as well as possible synergies with orbital observations. In a dedicated section, we describe the seismic impact of atmospheric phenomena (from the point of view of both noise'' to be decorrelated from the seismic signal and signal'' to provide information on atmospheric processes). We discuss in this framework Planetary Boundary Layer turbulence, with a focus on convective vortices and dust devils, gravity waves (with idealized modeling), and large-scale circulations. Our paper also presents possible new, exploratory, studies with the InSight instrumentation: surface layer scaling and exploration of the Monin-Obukhov model, aeolian surface changes and saltation / lifing studies, and monitoring of secular pressure changes. The InSight mission will be instrumental in broadening the knowledge of the Martian atmosphere, with a unique set of measurements from the surface of Mars. }}, doi = {10.1007/s11214-018-0543-0}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018SSRv..214..109S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018P&SS..161...26R, author = {{Read}, W.~G. and {Tamppari}, L.~K. and {Livesey}, N.~J. and {Clancy}, R.~T. and {Forget}, F. and {Hartogh}, P. and {Rafkin}, S.~C.~R. and {Chattopadhyay}, G.}, title = {{Retrieval of wind, temperature, water vapor and other trace constituents in the Martian Atmosphere}}, journal = {\planss}, keywords = {Mars, Atmosphere, Wind, Isotopes, Temperature, Humidity, Composition}, year = 2018, volume = 161, pages = {26-40}, abstract = {{Atmospheric limb sounding is a well-established technique for measuring atmospheric temperature, composition, and wind. The theoretical capabilities of a submillimeter limb sounder placed in low Mars orbit are quantified, with a particular focus on the ability to make profile measurements of line-of-sight wind, temperature, water vapor, deuterated water vapor, several isotopes of carbon monoxide, oxygen-18 carbon dioxide, ozone, and hydrogen peroxide. We identify cases where all such measurements can be made within a single 25-70 GHz wide region of the submillimeter spectrum, enabling use of a single state-of-the-art submillimeter receiver. Six potential spectral regions, approximately centered at 335 GHz, 450 GHz, 550 GHz, 900 GHz, 1000 GHz, and 1130 GHz are found, any one of which can provide a complete measurement suite. The expected precision and vertical resolution of temperature, composition, and wind measurements from instruments in each range are quantified. This work thus follows on from that of Urban et al. (2005), Kasai et al. (2012), and earlier studies, expanding them to consider many alternative observing frequency regions. In general, performance (in terms of measurement precision and vertical resolution) is improved with increasing observation frequency. In part this is due to our choice to assume the same antenna size for each frequency, thus providing a narrower field of view for the higher frequency configurations. The general increase in emission line strengths with increasing frequency also contributes to this improved performance in some cases. However, increased instrument power needs for the higher frequency configurations may argue against their choice in some mission scenarios. }}, doi = {10.1016/j.pss.2018.05.004}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018P%26SS..161...26R}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018NatGe..11..965N, author = {{Navarro}, T. and {Schubert}, G. and {Lebonnois}, S.}, title = {{Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate}}, journal = {Nature Geoscience}, year = 2018, volume = 11, pages = {965-965}, abstract = {{In the version of this Article originally published, a statement regarding past measurements of the length of day and rotation rate of Venus was potentially misleading. The original statement has now been replaced in the online versions of this Article, to acknowledge that neither Magellan nor Venus Express measured an instantaneous rotation rate. }}, doi = {10.1038/s41561-018-0257-7}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018NatGe..11..965N}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123.2773L, author = {{Lefèvre}, M. and {Lebonnois}, S. and {Spiga}, A.}, title = {{Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {Venus, modeling, convection, gravity waves}, year = 2018, volume = 123, pages = {2773-2789}, abstract = {{Venus' convective cloud layers and associated gravity waves strongly impact the local and global budget of heat, momentum, and chemical species. Here we use for the first time three-dimensional turbulence-resolving dynamical integrations of Venus' atmosphere from the surface to 100-km altitude, coupled with fully interactive radiative transfer computations. We show that this enables to correctly reproduce the vertical position (46- to 55-km altitude) and thickness (9 km) of the main convective cloud layer measured by Venus Express and Akatsuki radio occultations, as well as the intensity of convective plumes (3 m/s) measured by VEGA balloons. Both the radiative forcing in the visible and the large-scale dynamical impact play a role in the variability of the cloud convective activity with local time and latitude. Our model reproduces the diurnal cycle in cloud convection observed by Akatsuki at the low latitudes and the lack thereof observed by Venus Express at the equator. The observed enhancement of cloud convection at high latitudes is simulated by our model, although underestimated compared to observations. We show that the influence of the vertical shear of horizontal superrotating winds must be accounted for in our model to allow for gravity waves of the observed intensity ($\gt$1 K) and horizontal wavelength (up to 20 km) to be generated through the obstacle effect mechanism. The vertical extent of our model also allows us to predict for the first time a 7-km-thick convective layer at the cloud top (70-km altitude) caused by the solar absorption of the unknown ultraviolet absorber. }}, doi = {10.1029/2018JE005679}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123.2773L}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018AsBio..18.1221Y, author = {{Yung}, Y.~L. and {Chen}, P. and {Nealson}, K. and {Atreya}, S. and {Beckett}, P. and {Blank}, J.~G. and {Ehlmann}, B. and {Eiler}, J. and {Etiope}, G. and {Ferry}, J.~G. and {Forget}, F. and {Gao}, P. and {Hu}, R. and {Kleinb{\"o}hl}, A. and {Klusman}, R. and {Lefèvre}, F. and {Miller}, C. and {Mischna}, M. and {Mumma}, M. and {Newman}, S. and {Oehler}, D. and {Okumura}, M. and {Oremland}, R. and {Orphan}, V. and {Popa}, R. and {Russell}, M. and {Shen}, L. and {Sherwood Lollar}, B. and {Staehle}, R. and {Stamenkovi{\'c}}, V. and {Stolper}, D. and {Templeton}, A. and {Vandaele}, A.~C. and {Viscardy}, S. and {Webster}, C.~R. and {Wennberg}, P.~O. and {Wong}, M.~L. and {Worden}, J.}, title = {{Methane on Mars and Habitability: Challenges and Responses}}, journal = {Astrobiology}, year = 2018, volume = 18, pages = {1221-1242}, abstract = {{Recent measurements of methane (CH$_{4}$) by the Mars Science Laboratory (MSL) now confront us with robust data that demand interpretation. Thus far, the MSL data have revealed a baseline level of CH$_{4}$({\tilde}0.4 parts per billion by volume [ppbv]), with seasonal variations, as well as greatly enhanced spikes of CH$_{4}$with peak abundances of {\tilde}7 ppbv. What do these CH$_{4}$revelations with drastically different abundances and temporal signatures represent in terms of interior geochemical processes, or is martian CH$_{4}$a biosignature? Discerning how CH$_{4}$generation occurs on Mars may shed light on the potential habitability of Mars. There is no evidence of life on the surface of Mars today, but microbes might reside beneath the surface. In this case, the carbon flux represented by CH$_{4}$would serve as a link between a putative subterranean biosphere on Mars and what we can measure above the surface. Alternatively, CH$_{4}$records modern geochemical activity. Here we ask the fundamental question: how active is Mars, geochemically and/or biologically? In this article, we examine geological, geochemical, and biogeochemical processes related to our overarching question. The martian atmosphere and surface are an overwhelmingly oxidizing environment, and life requires pairing of electron donors and electron acceptors, that is, redox gradients, as an essential source of energy. Therefore, a fundamental and critical question regarding the possibility of life on Mars is, Where can we find redox gradients as energy sources for life on Mars?'' Hence, regardless of the pathway that generates CH$_{4}$on Mars, the presence of CH$_{4}$, a reduced species in an oxidant-rich environment, suggests the possibility of redox gradients supporting life and habitability on Mars. Recent missions such as ExoMars Trace Gas Orbiter may provide mapping of the global distribution of CH$_{4}$. To discriminate between abiotic and biotic sources of CH$_{4}$on Mars, future studies should use a series of diagnostic geochemical analyses, preferably performed below the ground or at the ground/atmosphere interface, including measurements of CH$_{4}$isotopes, methane/ethane ratios, H$_{2}$gas concentration, and species such as acetic acid. Advances in the fields of Mars exploration and instrumentation will be driven, augmented, and supported by an improved understanding of atmospheric chemistry and dynamics, deep subsurface biogeochemistry, astrobiology, planetary geology, and geophysics. Future Mars exploration programs will have to expand the integration of complementary areas of expertise to generate synergistic and innovative ideas to realize breakthroughs in advancing our understanding of the potential of life and habitable conditions having existed on Mars. In this spirit, we conducted a set of interdisciplinary workshops. From this series has emerged a vision of technological, theoretical, and methodological innovations to explore the martian subsurface and to enhance spatial tracking of key volatiles, such as CH$_{4}$. }}, doi = {10.1089/ast.2018.1917}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018AsBio..18.1221Y}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018SSRv..214..103E, author = {{Esposito}, F. and {Debei}, S. and {Bettanini}, C. and {Molfese}, C. and {Arruego Rodr{\'{\i}}guez}, I. and {Colombatti}, G. and {Harri}, A.-M. and {Montmessin}, F. and {Wilson}, C. and {Aboudan}, A. and {Schipani}, P. and {Marty}, L. and {{\'A}lvarez}, F.~J. and {Apestigue}, V. and {Bellucci}, G. and {Berthelier}, J.-J. and {Brucato}, J.~R. and {Calcutt}, S.~B. and {Chiodini}, S. and {Cortecchia}, F. and {Cozzolino}, F. and {Cucciarrè}, F. and {Deniskina}, N. and {Déprez}, G. and {Di Achille}, G. and {Ferri}, F. and {Forget}, F. and {Franzese}, G. and {Friso}, E. and {Genzer}, M. and {Hassen-Kodja}, R. and {Haukka}, H. and {Hieta}, M. and {Jiménez}, J.~J. and {Josset}, J.-L. and {Kahanp{\"a}{\"a}}, H. and {Karatekin}, O. and {Landis}, G. and {Lapauw}, L. and {Lorenz}, R. and {Martinez-Oter}, J. and {Mennella}, V. and {M{\"o}hlmann}, D. and {Moirin}, D. and {Molinaro}, R. and {Nikkanen}, T. and {Palomba}, E. and {Patel}, M.~R. and {Pommereau}, J.-P. and {Popa}, C.~I. and {Rafkin}, S. and {Rannou}, P. and {Renno}, N.~O. and {Rivas}, J. and {Schmidt}, W. and {Segato}, E. and {Silvestro}, S. and {Spiga}, A. and {Toledo}, D. and {Trautner}, R. and {Valero}, F. and {V{\'a}zquez}, L. and {Vivat}, F. and {Witasse}, O. and {Yela}, M. and {Mugnuolo}, R. and {Marchetti}, E. and {Pirrotta}, S.}, title = {{The DREAMS Experiment Onboard the Schiaparelli Module of the ExoMars 2016 Mission: Design, Performances and Expected Results}}, journal = {\ssr}, keywords = {ExoMars, Schiaparelli, DREAMS, Mars, Atmospheric electric field, Meteorological station, Dust storm season}, year = 2018, volume = 214, eid = {103}, pages = {103}, abstract = {{The first of the two missions foreseen in the ExoMars program was successfully launched on 14th March 2016. It included the Trace Gas Orbiter and the Schiaparelli Entry descent and landing Demonstrator Module. Schiaparelli hosted the DREAMS instrument suite that was the only scientific payload designed to operate after the touchdown. DREAMS is a meteorological station with the capability of measuring the electric properties of the Martian atmosphere. It was a completely autonomous instrument, relying on its internal battery for the power supply. Even with low resources (mass, energy), DREAMS would be able to perform novel measurements on Mars (atmospheric electric field) and further our understanding of the Martian environment, including the dust cycle. DREAMS sensors were designed to operate in a very dusty environment, because the experiment was designed to operate on Mars during the dust storm season (October 2016 in Meridiani Planum). Unfortunately, the Schiaparelli module failed part of the descent and the landing and crashed onto the surface of Mars. Nevertheless, several seconds before the crash, the module central computer switched the DREAMS instrument on, and sent back housekeeping data indicating that the DREAMS sensors were performing nominally. This article describes the instrument in terms of scientific goals, design, working principle and performances, as well as the results of calibration and field tests. The spare model is mature and available to fly in a future mission. }}, doi = {10.1007/s11214-018-0535-0}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018SSRv..214..103E}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018SSRv..214...84G, author = {{Golombek}, M. and {Grott}, M. and {Kargl}, G. and {Andrade}, J. and {Marshall}, J. and {Warner}, N. and {Teanby}, N.~A. and {Ansan}, V. and {Hauber}, E. and {Voigt}, J. and {Lichtenheldt}, R. and {Knapmeyer-Endrun}, B. and {Daubar}, I.~J. and {Kipp}, D. and {Muller}, N. and {Lognonné}, P. and {Schmelzbach}, C. and {Banfield}, D. and {Trebi-Ollennu}, A. and {Maki}, J. and {Kedar}, S. and {Mimoun}, D. and {Murdoch}, N. and {Piqueux}, S. and {Delage}, P. and {Pike}, W.~T. and {Charalambous}, C. and {Lorenz}, R. and {Fayon}, L. and {Lucas}, A. and {Rodriguez}, S. and {Morgan}, P. and {Spiga}, A. and {Panning}, M. and {Spohn}, T. and {Smrekar}, S. and {Gudkova}, T. and {Garcia}, R. and {Giardini}, D. and {Christensen}, U. and {Nicollier}, T. and {Sollberger}, D. and {Robertsson}, J. and {Ali}, K. and {Kenda}, B. and {Banerdt}, W.~B. }, title = {{Geology and Physical Properties Investigations by the InSight Lander}}, journal = {\ssr}, keywords = {InSight, Mars, Geology, Physical properties, Surface materials}, year = 2018, volume = 214, eid = {84}, pages = {84}, abstract = {{Although not the prime focus of the InSight mission, the near-surface geology and physical properties investigations provide critical information for both placing the instruments (seismometer and heat flow probe with mole) on the surface and for understanding the nature of the shallow subsurface and its effect on recorded seismic waves. Two color cameras on the lander will obtain multiple stereo images of the surface and its interaction with the spacecraft. Images will be used to identify the geologic materials and features present, quantify their areal coverage, help determine the basic geologic evolution of the area, and provide ground truth for orbital remote sensing data. A radiometer will measure the hourly temperature of the surface in two spots, which will determine the thermal inertia of the surface materials present and their particle size and/or cohesion. Continuous measurements of wind speed and direction offer a unique opportunity to correlate dust devils and high winds with eolian changes imaged at the surface and to determine the threshold friction wind stress for grain motion on Mars. During the first two weeks after landing, these investigations will support the selection of instrument placement locations that are relatively smooth, flat, free of small rocks and load bearing. Soil mechanics parameters and elastic properties of near surface materials will be determined from mole penetration and thermal conductivity measurements from the surface to 3-5 m depth, the measurement of seismic waves during mole hammering, passive monitoring of seismic waves, and experiments with the arm and scoop of the lander (indentations, scraping and trenching). These investigations will determine and test the presence and mechanical properties of the expected 3-17 m thick fragmented regolith (and underlying fractured material) built up by impact and eolian processes on top of Hesperian lava flows and determine its seismic properties for the seismic investigation of Mars' interior. }}, doi = {10.1007/s11214-018-0512-7}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018SSRv..214...84G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JQSRT.213..178H, author = {{Hartmann}, J.-M. and {Tran}, H. and {Armante}, R. and {Boulet}, C. and {Campargue}, A. and {Forget}, F. and {Gianfrani}, L. and {Gordon}, I. and {Guerlet}, S. and {Gustafsson}, M. and {Hodges}, J.~T. and {Kassi}, S. and {Lisak}, D. and {Thibault}, F. and {Toon}, G.~C.}, title = {{Recent advances in collisional effects on spectra of molecular gases and their practical consequences}}, journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}, keywords = {Pressure effects on spectral shapes, Experimental techniques, Theories and models, Available data, Consequences for applications}, year = 2018, volume = 213, pages = {178-227}, abstract = {{We review progress, since publication of the book Collisional effects on molecular spectra: Laboratory experiments and models, consequences for applications (Elsevier, Amsterdam, 2008), on measuring, modeling and predicting the influence of pressure (ie of intermolecular collisions) on the spectra of gas molecules. We first introduce recently developed experimental techniques of high accuracy and sensitivity. We then complement the aforementioned book by presenting the theoretical approaches, results and data proposed (mostly) in the last decade on the topics of isolated line shapes, line-broadening and -shifting, line-mixing, the far wings and associated continua, and collision-induced absorption. Examples of recently demonstrated consequences of the progress in the description of spectral shapes for some practical applications (metrology, probing of gas media, climate predictions) are then given. Remaining issues and directions for future research are finally discussed. }}, doi = {10.1016/j.jqsrt.2018.03.016}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JQSRT.213..178H}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123.1934G, author = {{Gonz{\'a}lez-Galindo}, F. and {Chaufray}, J.-Y. and {Forget}, F. and {Garc{\'{\i}}a-Comas}, M. and {Montmessin}, F. and {Jain}, S.~K. and {Stiepen}, A.}, title = {{UV Dayglow Variability on Mars: Simulation With a Global Climate Model and Comparison With SPICAM/MEx Data}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {Mars, dayglow, global modeling, Mars Express}, year = 2018, volume = 123, pages = {1934-1952}, abstract = {{A model able to simulate the CO Cameron bands and the CO$_{2}^{+} UV doublet, two of the most prominent UV emissions in the Martian dayside, has been incorporated into a Mars global climate model. The model self-consistently quantifies the effects of atmospheric variability on the simulated dayglow for the first time. Comparison of the modeled peak intensities with Mars Express (MEx) SPICAM (Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars) observations confirms previous suggestions that electron impact cross sections on CO_{2} and CO need to be reduced. The peak altitudes are well predicted by the model, except for the period of MY28 characterized by the presence of a global dust storm. Global maps of the simulated emission systems have been produced, showing a seasonal variability of the peak intensities dominated by the eccentricity of the Martian orbit. A significant contribution of the CO electron impact excitation to the Cameron bands is found, with variability linked to that of the CO abundance. This is in disagreement with previous theoretical models, due to the larger CO abundance predicted by our model. In addition, the contribution of this process increases with altitude, indicating that care should be taken when trying to derive temperatures from the scale height of this emission. The analysis of the geographical variability of the predicted intensities reflects the predicted density variability. In particular, a longitudinal variability dominated by a wave-3 pattern is obtained both in the predicted density and in the predicted peak altitudes. }}, doi = {10.1029/2018JE005556}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123.1934G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..309..277B, author = {{Bertrand}, T. and {Forget}, F. and {Umurhan}, O.~M. and {Grundy}, W.~M. and {Schmitt}, B. and {Protopapa}, S. and {Zangari}, A.~M. and {White}, O.~L. and {Schenk}, P.~M. and {Singer}, K.~N. and {Stern}, A. and {Weaver}, H.~A. and {Young}, L.~A. and {Ennico}, K. and {Olkin}, C.~B.}, title = {{The nitrogen cycles on Pluto over seasonal and astronomical timescales}}, journal = {\icarus}, archiveprefix = {arXiv}, eprint = {1804.02434}, primaryclass = {astro-ph.EP}, keywords = {Pluto, Nitrogen, Paleo, Modeling, GCM, Sputnik Planitia}, year = 2018, volume = 309, pages = {277-296}, abstract = {{Pluto's landscape is shaped by the endless condensation and sublimation cycles of the volatile ices covering its surface. In particular, the Sputnik Planitia ice sheet, which is thought to be the main reservoir of nitrogen ice, displays a large diversity of terrains, with bright and dark plains, small pits and troughs, topographic depressions and evidences of recent and past glacial flows. Outside Sputnik Planitia, New Horizons also revealed numerous nitrogen ice deposits, in the eastern side of Tombaugh Regio and at mid-northern latitudes. These observations suggest a complex history involving volatile and glacial processes occurring on different timescales. We present numerical simulations of volatile transport on Pluto performed with a model designed to simulate the nitrogen cycle over millions of years, taking into account the changes of obliquity, solar longitude of perihelion and eccentricity as experienced by Pluto. Using this model, we first explore how the volatile and glacial activity of nitrogen within Sputnik Planitia has been impacted by the diurnal, seasonal and astronomical cycles of Pluto. Results show that the obliquity dominates the N_{2} cycle and that over one obliquity cycle, the latitudes of Sputnik Planitia between 25{\deg}S-30{\deg}N are dominated by N_{2} condensation, while the northern regions between 30{\deg}N and -50{\deg}N are dominated by N_{2} sublimation. We find that a net amount of 1 km of ice has sublimed at the northern edge of Sputnik Planitia during the last 2 millions of years. It must have been compensated by a viscous flow of the thick ice sheet. By comparing these results with the observed geology of Sputnik Planitia, we can relate the formation of the small pits and the brightness of the ice at the center of Sputnik Planitia to the sublimation and condensation of ice occurring at the annual timescale, while the glacial flows at its eastern edge and the erosion of the water ice mountains all around the ice sheet are instead related to the astronomical timescale. We also perform simulations including a glacial flow scheme which shows that the Sputnik Planitia ice sheet is currently at its minimum extent at the northern and southern edges. We also explore the stability of N_{2} ice deposits outside the latitudes and longitudes of the Sputnik Planitia basin. Results show that N_{2} ice is not stable at the poles but rather in the equatorial regions, in particular in depressions, where thick deposits may persist over tens of millions of years, before being trapped in Sputnik Planitia. Finally, another key result is that the minimum and maximum surface pressures obtained over the simulated millions of years remain in the range of milli-Pascals and Pascals, respectively. This suggests that Pluto never encountered conditions allowing liquid nitrogen to flow directly on its surface. Instead, we suggest that the numerous geomorphological evidences of past liquid flow observed on Pluto's surface are the result of liquid nitrogen that flowed at the base of thick ancient nitrogen glaciers, which have since disappeared. }}, doi = {10.1016/j.icarus.2018.03.012}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..309..277B}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..308..197S, author = {{Spiga}, A. and {Smith}, I.}, title = {{Katabatic jumps in the Martian northern polar regions}}, journal = {\icarus}, year = 2018, volume = 308, pages = {197-208}, abstract = {{Martian polar regions host active regional wind circulations, such as the downslope katabatic winds which develop owing to near-surface radiative cooling and sloped topography. Many observations (stratigraphy from radar profiling, frost streaks, spectral analysis of ices) concur to show that aeolian processes play a key role in glacial processes in Martian polar regions. A spectacular manifestation of this resides in elongated clouds that forms within the polar spiral troughs, a series of geological depressions in Mars' polar caps. Here we report mesoscale atmospheric modeling in Martian polar regions making use of five nested domains operating a model downscaling from horizontal resolutions of twenty kilometers to 200 m in a typical polar trough. We show that strong katabatic jumps form at the bottom of polar troughs with an horizontal morphology and location similar to trough clouds, large vertical velocity (up to +3 m/s) and temperature perturbations (up to 20 K) propitious to cloud formation. This strongly suggests that trough clouds on Mars are caused by katabatic jumps forming within polar troughs. This phenomena is analogous to the terrestrial Loewe phenomena over Antarctica's slopes and coastlines, resulting in a distinctive wall of snow'' during katabatic events. Our mesoscale modeling results thereby suggest that trough clouds might be present manifestations of the ice migration processes that yielded the internal cap structure discovered by radar observations, as part of a cyclic step'' process. This has important implications for the stability and possible migration over geological timescales of water ice surface reservoirs-and, overall, for the evolution of Mars' polar caps over geological timescales. }}, doi = {10.1016/j.icarus.2017.10.021}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..308..197S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..308..188S, author = {{Smith}, I.~B. and {Spiga}, A.}, title = {{Seasonal variability in winds in the north polar region of Mars}}, journal = {\icarus}, year = 2018, volume = 308, pages = {188-196}, abstract = {{Surface features near Mars' polar regions are very active, suggesting that they are among the most dynamic places on the planet. Much of that activity is driven by seasonal winds that strongly influence the distribution of water ice and other particulates. Morphologic features such as the spiral troughs, Chasma Boreale, and prominent circumpolar dune fields have experienced persistent winds for several Myr. Therefore, detailing the pattern of winds throughout the year is an important step to understanding what processes affect the martian surface in contemporary and past epochs. In this study, we provide polar-focused mesoscale simulations from northern spring to summer to understand variability from the diurnal to the seasonal scales. We find that there is a strong seasonality to the diurnal surface wind speeds driven primarily by the retreat of the seasonal CO_{2} until about summer solstice, when the CO_{2} is gone. The fastest winds are found when the CO_{2} cap boundary is on the slopes of the north polar layered deposits, providing a strong thermal gradient that enhances the season-long katabatic effect. Mid-summer winds, while not as fast as spring winds, may play a role in dune migration for some dune fields. Late summer wind speeds pick up as the seasonal cap returns. }}, doi = {10.1016/j.icarus.2017.10.005}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..308..188S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..308...76G, author = {{Guallini}, L. and {Rossi}, A.~P. and {Forget}, F. and {Marinangeli}, L. and {Lauro}, S.~E. and {Pettinelli}, E. and {Seu}, R. and {Thomas}, N. }, title = {{Regional stratigraphy of the south polar layered deposits (Promethei Lingula, Mars): Discontinuity-bounded'' units in images and radargrams}}, journal = {\icarus}, keywords = {Geological processes, Mars, polar geology, surface, Image processing}, year = 2018, volume = 308, pages = {76-107}, abstract = {{The Mars South Polar Layered Deposits (SPLD) are the result of depositional and erosional events, which are marked by different stratigraphic sequences and erosional surfaces. To unambiguously define the stratigraphic units at regional scale, we mapped the SPLD on the basis of observed discontinuities (i.e., unconformities, correlative discontinuities and conformities), as commonly done in terrestrial modern stratigraphy. This methodology is defined as Discontinuity-Bounded Units'' or allostratigraphy, and is complemented by geomorphological mapping. Our study focuses on Promethei Lingula (PL) and uses both high-resolution images (CTX, HiRISE) and radargrams (SHARAD) to combine surface and sub-surface observations and obtain a 3D geological reconstruction of the SPLD. One regional discontinuity (named AUR1) was defined within the studied stratigraphic succession and is exposed in several non-contiguous outcrops around PL as well as observed at depth within the ice sheet. This is the primary contact between two major depositional sequences, showing a different texture at CTX resolution. The lower sequence is characterized mainly by a ridge and trough'' morphology (Ridge and Trough Sequence; RTS) and the upper sequence shows mainly by a stair-stepped'' morphology (Stair-Stepped Sequence; SSS). On the basis of the observations, we defined two regional discontinuity-bounded'' units in PL, respectively coinciding with RTS and SSS sequences. Our stratigraphic reconstruction provides new hints on the major scale events that shaped this region. Oscillations in Martian axial obliquity could have controlled local climate conditions in the past, affecting the PL geological record. }}, doi = {10.1016/j.icarus.2017.08.030}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..308...76G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..308....2S, author = {{Smith}, I.~B. and {Diniega}, S. and {Beaty}, D.~W. and {Thorsteinsson}, T. and {Becerra}, P. and {Bramson}, A.~M. and {Clifford}, S.~M. and {Hvidberg}, C.~S. and {Portyankina}, G. and {Piqueux}, S. and {Spiga}, A. and {Titus}, T.~N.}, title = {{6th international conference on Mars polar science and exploration: Conference summary and five top questions}}, journal = {\icarus}, year = 2018, volume = 308, pages = {2-14}, abstract = {{We provide a historical context of the International Conference on Mars Polar Science and Exploration and summarize the proceedings from the 6th iteration of this meeting. In particular, we identify five key Mars polar science questions based primarily on presentations and discussions at the conference and discuss the overlap between some of those questions. We briefly describe the seven scientific field trips that were offered at the conference, which greatly supplemented conference discussion of Mars polar processes and landforms. We end with suggestions for measurements, modeling, and laboratory and field work that were highlighted during conference discussion as necessary steps to address key knowledge gaps. }}, doi = {10.1016/j.icarus.2017.06.027}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..308....2S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Sci...360..992T, author = {{Telfer}, M.~W. and {Parteli}, E.~J.~R. and {Radebaugh}, J. and {Beyer}, R.~A. and {Bertrand}, T. and {Forget}, F. and {Nimmo}, F. and {Grundy}, W.~M. and {Moore}, J.~M. and {Stern}, S.~A. and {Spencer}, J. and {Lauer}, T.~R. and {Earle}, A.~M. and {Binzel}, R.~P. and {Weaver}, H.~A. and {Olkin}, C.~B. and {Young}, L.~A. and {Ennico}, K. and {Runyon}, K. and {aff12}}, title = {{Dunes on Pluto}}, journal = {Science}, year = 2018, volume = 360, pages = {992-997}, abstract = {{The surface of Pluto is more geologically diverse and dynamic than had been expected, but the role of its tenuous atmosphere in shaping the landscape remains unclear. We describe observations from the New Horizons spacecraft of regularly spaced, linear ridges whose morphology, distribution, and orientation are consistent with being transverse dunes. These are located close to mountainous regions and are orthogonal to nearby wind streaks. We demonstrate that the wavelength of the dunes (\~{}0.4 to 1 kilometer) is best explained by the deposition of sand-sized (\~{}200 to \~{}300 micrometer) particles of methane ice in moderate winds (\lt10 meters per second). The undisturbed morphology of the dunes, and relationships with the underlying convective glacial ice, imply that the dunes have formed in the very recent geological past. }}, doi = {10.1126/science.aao2975}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Sci...360..992T}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018NatGe..11..487N, author = {{Navarro}, T. and {Schubert}, G. and {Lebonnois}, S.}, title = {{Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate}}, journal = {Nature Geoscience}, year = 2018, volume = 11, pages = {487-491}, abstract = {{The Akatsuki spacecraft observed a 10,000-km-long meridional structure at the top of the cloud deck of Venus that appeared stationary with respect to the surface and was interpreted as a gravity wave. Additionally, over four Venus solar days of observations, other such waves were observed to appear in the afternoon over equatorial highland regions. This indicates a direct influence of the solid planet on the whole Venusian atmosphere despite dissimilar rotation rates of 243 and 4 days, respectively. How such gravity waves might be generated on Venus is not understood. Here, we use general circulation model simulations of the Venusian atmosphere to show that the observations are consistent with stationary gravity waves over topographic highs{\mdash}or mountain waves{\mdash}that are generated in the afternoon in equatorial regions by the diurnal cycle of near-surface atmospheric stability. We find that these mountain waves substantially contribute to the total atmospheric torque that acts on the planet's surface. We estimate that mountain waves, along with the thermal tide and baroclinic waves, can produce a change in the rotation rate of the solid body of about 2 minutes per solar day. This interplay between the solid planet and atmosphere may explain some of the difference in rotation rates (equivalent to a change in the length of day of about 7 minutes) measured by spacecraft over the past 40 years. }}, doi = {10.1038/s41561-018-0157-x}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018NatGe..11..487N}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123.1449G, author = {{Gr{\"o}ller}, H. and {Montmessin}, F. and {Yelle}, R.~V. and {Lefèvre}, F. and {Forget}, F. and {Schneider}, N.~M. and {Koskinen}, T.~T. and {Deighan}, J. and {Jain}, S.~K.}, title = {{MAVEN/IUVS Stellar Occultation Measurements of Mars Atmospheric Structure and Composition}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {MAVEN/IUVS stellar occultations, atmospheric composition and structure, temperature profiles, waves/tides detection, ozone, molecular oxygen}, year = 2018, volume = 123, pages = {1449-1483}, abstract = {{The Imaging UltraViolet Spectrograph (IUVS) instrument of the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission has acquired data on Mars for more than one Martian year. During this time, beginning with March 2015, hundreds of stellar occultations have been observed, in 12 dedicated occultation campaigns, executed on average every 2 to 3 and the full range longitude and local times with relatively sparse sampling. From these measurements we retrieve CO_{2}, O_{2}, and O_{3} number densities as well as temperature profiles in the altitude range from 20 to 160 km, covering 8 orders of magnitude in pressure from {\tilde}2 {\times} 10^{1} to {\tilde}4 {\times} 10^{-7} Pa. These data constrain the composition and thermal structure of the atmosphere. The O_{2} mixing ratios retrieved during this study show a high variability from 1.5 {\times} 10^{-3} to 6 {\times} 10^{-3}; however, the mean value seems to be constant with solar longitude. We detect ozone between 20 and 60 km. In many profiles there is a well-defined peak between 30 and 40 km with a maximum density of 1-2 {\times}10^{9} cm^{-3}. Examination of the vertical temperature profiles reveals substantial disagreement with models, with observed temperatures both warmer and colder than predicted. Examination of the altitude profiles of density perturbations and their variation with longitude shows structured atmospheric perturbations at altitudes above 100 km that are likely nonmigrating tides. These perturbations are dominated by zonal wave numbers 2 and 3 with amplitudes greater than 45\%. }}, doi = {10.1029/2017JE005466}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123.1449G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..307..161K, author = {{Koskinen}, T.~T. and {Guerlet}, S.}, title = {{Atmospheric structure and helium abundance on Saturn from Cassini/UVIS and CIRS observations}}, journal = {\icarus}, keywords = {Saturn, Occultations, Infrared observations, Atmospheres, Structure}, year = 2018, volume = 307, pages = {161-171}, abstract = {{We combine measurements from stellar occultations observed by the Cassini Ultraviolet Imaging Spectrograph (UVIS) and limb scans observed by the Composite Infrared Spectrometer (CIRS) to create empirical atmospheric structure models for Saturn corresponding to the locations probed by the occultations. The results cover multiple locations at low to mid-latitudes between the spring of 2005 and the fall of 2015. We connect the temperature-pressure (T-P) profiles retrieved from the CIRS limb scans in the stratosphere to the T-P profiles in the thermosphere retrieved from the UVIS occultations. We calculate the altitudes corresponding to the pressure levels in each case based on our best fit composition model that includes H_{2}, He, CH_{4} and upper limits on H. We match the altitude structure to the density profile in the thermosphere that is retrieved from the occultations. Our models depend on the abundance of helium and we derive a volume mixing ratio of 11 {\plusmn} 2\% for helium in the lower atmosphere based on a statistical analysis of the values derived for 32 different occultation locations. We also derive the mean temperature and methane profiles in the upper atmosphere and constrain their variability. Our results are consistent with enhanced heating at the polar auroral region and a dynamically active upper atmosphere. }}, doi = {10.1016/j.icarus.2018.02.020}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..307..161K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..306..116T, author = {{Tran}, H. and {Turbet}, M. and {Chelin}, P. and {Landsheere}, X. }, title = {{Measurements and modeling of absorption by CO_{2 }+ H_{2}O mixtures in the spectral region beyond the CO_{2} {\nu}_{3}-band head}}, journal = {\icarus}, archiveprefix = {arXiv}, eprint = {1802.01352}, primaryclass = {astro-ph.EP}, year = 2018, volume = 306, pages = {116-121}, abstract = {{In this work, we measured the absorption by CO_{2 }+ H_{2}O mixtures from 2400 to 2600 cm^{-1} which corresponds to the spectral region beyond the {\nu}_{3} band head of CO_{2}. Transmission spectra of CO_{2} mixed with water vapor were recorded with a high-resolution Fourier-transform spectrometer for various pressure, temperature and concentration conditions. The continuum absorption by CO_{2} due to the presence of water vapor was determined by subtracting from measured spectra the contribution of local lines of both species, that of the continuum of pure CO_{2} as well as of the self- and CO_{2}-continua of water vapor induced by the H_{2}O-H_{2}O and H_{2}O-CO_{2} interactions. The obtained results are in very good agreement with the unique previous measurement (in a narrower spectral range). They confirm that the H_{2}O-continuum of CO_{2} is significantly larger than that observed for pure CO_{2}. This continuum thus must be taken into account in radiative transfer calculations for media involving CO_{2}+ H_{2}O mixture. An empirical model, using sub-Lorentzian line shapes based on some temperature-dependent correction factors {\chi} is proposed which enables an accurate description of the experimental results. }}, doi = {10.1016/j.icarus.2018.02.009}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..306..116T}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018E&PSL.489..241F, author = {{Fernandez-Cascales}, L. and {Lucas}, A. and {Rodriguez}, S. and {Gao}, X. and {Spiga}, A. and {Narteau}, C.}, title = {{First quantification of relationship between dune orientation and sediment availability, Olympia Undae, Mars}}, journal = {Earth and Planetary Science Letters}, keywords = {Mars, dunes, bedform alignment, sediment cover, aeolian transport}, year = 2018, volume = 489, pages = {241-250}, abstract = {{Dunes provide unique information about wind regimes on planetary bodies where there is no direct meteorological data. At the eastern margin of Olympia Undae on Mars, dune orientation is measured from satellite imagery and sediment cover is estimated using the high contrast between the dune material and substrate. The analysis of these data provide the first quantification of relationship between sediment availability and dune orientation. Abrupt and smooth dune reorientations are associated with inward and outward dynamics of dunes approaching and ejecting from major sedimentary bodies, respectively. These reorientation patterns along sediment transport pathways are interpreted using a new generation dune model based on the coexistence of two dune growth mechanisms. This model also permits solving of the inverse problem of predicting the wind regime from dune orientation. For bidirectional wind regimes, solutions of this inverse problem show substantial differences in the distributions of sediment flux orientation, which can be attributed to atmospheric flow variations induced by changes in albedo at the boundaries of major dune fields. Then, we conclude that relationships between sediment cover and dune orientation can be used to constrain wind regime and dune field development on Mars and other planetary surfaces. }}, doi = {10.1016/j.epsl.2018.03.001}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018E%26PSL.489..241F}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018AREPS..46..175R, author = {{Read}, P.~L. and {Lebonnois}, S.}, title = {{Superrotation on Venus, on Titan, and Elsewhere}}, journal = {Annual Review of Earth and Planetary Sciences}, year = 2018, volume = 46, pages = {175-202}, abstract = {{The superrotation of the atmospheres of Venus and Titan has puzzled dynamicists for many years and seems to put these planets in a very different dynamical regime from most other planets. In this review, we consider how to define superrotation objectively and explore the constraints that determine its occurrence. Atmospheric superrotation also occurs elsewhere in the Solar System and beyond, and we compare Venus and Titan with Earth and other planets for which wind estimates are available. The extreme superrotation on Venus and Titan poses some difficult challenges for numerical models of atmospheric circulation, much more difficult than for more rapidly rotating planets such as Earth or Mars. We consider mechanisms for generating and maintaining a superrotating state, all of which involve a global meridional overturning circulation. The role of nonaxisymmetric eddies is crucial, however, but the detailed mechanisms may differ between Venus, Titan, and other planets. }}, doi = {10.1146/annurev-earth-082517-010137}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018AREPS..46..175R}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018A&A...613A..68G, author = {{Grimm}, S.~L. and {Demory}, B.-O. and {Gillon}, M. and {Dorn}, C. and {Agol}, E. and {Burdanov}, A. and {Delrez}, L. and {Sestovic}, M. and {Triaud}, A.~H.~M.~J. and {Turbet}, M. and {Bolmont}, {\'E}. and {Caldas}, A. and {de Wit}, J. and {Jehin}, E. and {Leconte}, J. and {Raymond}, S.~N. and {Van Grootel}, V. and {Burgasser}, A.~J. and {Carey}, S. and {Fabrycky}, D. and {Heng}, K. and {Hernandez}, D.~M. and {Ingalls}, J.~G. and {Lederer}, S. and {Selsis}, F. and {Queloz}, D. }, title = {{The nature of the TRAPPIST-1 exoplanets}}, journal = {\aap}, archiveprefix = {arXiv}, eprint = {1802.01377}, primaryclass = {astro-ph.EP}, keywords = {methods: numerical, planets and satellites: detection, planets and satellites: individual: TRAPPIST-1}, year = 2018, volume = 613, eid = {A68}, pages = {A68}, abstract = {{Context. The TRAPPIST-1 system hosts seven Earth-sized, temperate exoplanets orbiting an ultra-cool dwarf star. As such, it represents a remarkable setting to study the formation and evolution of terrestrial planets that formed in the same protoplanetary disk. While the sizes of the TRAPPIST-1 planets are all known to better than 5\% precision, their densities have significant uncertainties (between 28\% and 95\%) because of poor constraints on the planet's masses. Aims: The goal of this paper is to improve our knowledge of the TRAPPIST-1 planetary masses and densities using transit-timing variations (TTVs). The complexity of the TTV inversion problem is known to be particularly acute in multi-planetary systems (convergence issues, degeneracies and size of the parameter space), especially for resonant chain systems such as TRAPPIST-1. Methods: To overcome these challenges, we have used a novel method that employs a genetic algorithm coupled to a full N-body integrator that we applied to a set of 284 individual transit timings. This approach enables us to efficiently explore the parameter space and to derive reliable masses and densities from TTVs for all seven planets. Results: Our new masses result in a five- to eight-fold improvement on the planetary density uncertainties, with precisions ranging from 5\% to 12\%. These updated values provide new insights into the bulk structure of the TRAPPIST-1 planets. We find that TRAPPIST-1 c and e likely have largely rocky interiors, while planets b, d, f, g, and h require envelopes of volatiles in the form of thick atmospheres, oceans, or ice, in most cases with water mass fractions less than 5\%. }}, doi = {10.1051/0004-6361/201732233}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...613A..68G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018A&A...612A..86T, author = {{Turbet}, M. and {Bolmont}, E. and {Leconte}, J. and {Forget}, F. and {Selsis}, F. and {Tobie}, G. and {Caldas}, A. and {Naar}, J. and {Gillon}, M.}, title = {{Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets}}, journal = {\aap}, archiveprefix = {arXiv}, eprint = {1707.06927}, primaryclass = {astro-ph.EP}, keywords = {stars: individual: TRAPPIST-1, planets and satellites: terrestrial planets, planets and satellites: atmospheres, planets and satellites: dynamical evolution and stability, astrobiology}, year = 2018, volume = 612, eid = {A86}, pages = {A86}, abstract = {{TRAPPIST-1 planets are invaluable for the study of comparative planetary science outside our solar system and possibly habitability. Both transit timing variations (TTV) of the planets and the compact, resonant architecture of the system suggest that TRAPPIST-1 planets could be endowed with various volatiles today. First, we derived from N-body simulations possible planetary evolution scenarios, and show that all the planets are likely in synchronous rotation. We then used a versatile 3D global climate model (GCM) to explore the possible climates of cool planets around cool stars, with a focus on the TRAPPIST-1 system. We investigated the conditions required for cool planets to prevent possible volatile species to be lost permanently by surface condensation, irreversible burying or photochemical destruction. We also explored the resilience of the same volatiles (when in condensed phase) to a runaway greenhouse process. We find that background atmospheres made of N_{2}, CO, or O_{2} are rather resistant to atmospheric collapse. However, even if TRAPPIST-1 planets were able to sustain a thick background atmosphere by surviving early X/EUV radiation and stellar wind atmospheric erosion, it is difficult for them to accumulate significant greenhouse gases like CO_{2}, CH_{4}, or NH_{3}. CO_{2} can easily condense on the permanent nightside, forming CO_{2} ice glaciers that would flow toward the substellar region. A complete CO_{2} ice surface cover is theoretically possible on TRAPPIST-1g and h only, but CO_{2} ices should be gravitationally unstable and get buried beneath the water ice shell in geologically short timescales. Given TRAPPIST-1 planets large EUV irradiation (at least 10^{3} {\times} Titan's flux), CH_{4} and NH_{3} are photodissociated rapidly and are thus hard to accumulate in the atmosphere. Photochemical hazes could then sedimentate and form a surface layer of tholins that would progressively thicken over the age of the TRAPPIST-1 system. Regarding habitability, we confirm that few bars of CO_{2} would suffice to warm the surface of TRAPPIST-1f and g above the melting point of water. We also show that TRAPPIST-1e is a remarkable candidate for surface habitability. If the planet is today synchronous and abundant in water, then it should very likely sustain surface liquid water at least in the substellar region, whatever the atmosphere considered. }}, doi = {10.1051/0004-6361/201731620}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...612A..86T}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123..982W, author = {{Wang}, C. and {Forget}, F. and {Bertrand}, T. and {Spiga}, A. and {Millour}, E. and {Navarro}, T.}, title = {{Parameterization of Rocket Dust Storms on Mars in the LMD Martian GCM: Modeling Details and Validation}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {rocket dust storm, detached dust layers, parameterization, LMD Martian GCM, MCS}, year = 2018, volume = 123, pages = {982-1000}, abstract = {{The origin of the detached dust layers observed by the Mars Climate Sounder aboard the Mars Reconnaissance Orbiter is still debated. Spiga et al. (2013, https://doi.org/10.1002/jgre.20046) revealed that deep mesoscale convective rocket dust storms'' are likely to play an important role in forming these dust layers. To investigate how the detached dust layers are generated by this mesoscale phenomenon and subsequently evolve at larger scales, a parameterization of rocket dust storms to represent the mesoscale dust convection is designed and included into the Laboratoire de Météorologie Dynamique (LMD) Martian Global Climate Model (GCM). The new parameterization allows dust particles in the GCM to be transported to higher altitudes than in traditional GCMs. Combined with the horizontal transport by large-scale winds, the dust particles spread out and form detached dust layers. During the Martian dusty seasons, the LMD GCM with the new parameterization is able to form detached dust layers. The formation, evolution, and decay of the simulated dust layers are largely in agreement with the Mars Climate Sounder observations. This suggests that mesoscale rocket dust storms are among the key factors to explain the observed detached dust layers on Mars. However, the detached dust layers remain absent in the GCM during the clear seasons, even with the new parameterization. This implies that other relevant atmospheric processes, operating when no dust storms are occurring, are needed to explain the Martian detached dust layers. More observations of local dust storms could improve the ad hoc aspects of this parameterization, such as the trigger and timing of dust injection. }}, doi = {10.1002/2017JE005255}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123..982W}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123..780S, author = {{Singh}, D. and {Flanner}, M.~G. and {Millour}, E.}, title = {{Improvement of Mars Surface Snow Albedo Modeling in LMD Mars GCM With SNICAR}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {Mars, snow modeling, cryosphere, LMD Mars GCM}, year = 2018, volume = 123, pages = {780-791}, abstract = {{The current version of Laboratoire de Météorologie Dynamique (LMD) Mars GCM (original-MGCM) uses annually repeating (prescribed) CO_{2} snow albedo values based on the Thermal Emission Spectrometer observations. We integrate the Snow, Ice, and Aerosol Radiation (SNICAR) model with MGCM (SNICAR-MGCM) to prognostically determine H_{2}O and CO_{2} snow albedos interactively in the model. Using the new diagnostic capabilities of this model, we find that cryospheric surfaces (with dust) increase the global surface albedo of Mars by 0.022. Over snow-covered regions, SNICAR-MGCM simulates mean albedo that is higher by about 0.034 than prescribed values in the original-MGCM. Globally, shortwave flux into the surface decreases by 1.26 W/m^{2}, and net CO_{2} snow deposition increases by about 4\% with SNICAR-MGCM over one Martian annual cycle as compared to the original-MGCM simulations. SNICAR integration reduces the mean global surface temperature and the surface pressure of Mars by about 0.87\% and 2.5\%, respectively. Changes in albedo also show a similar distribution to dust deposition over the globe. The SNICAR-MGCM model generates albedos with higher sensitivity to surface dust content as compared to original-MGCM. For snow-covered regions, we improve the correlation between albedo and optical depth of dust from -0.91 to -0.97 with SNICAR-MGCM as compared to the original-MGCM. Dust substantially darkens Mars's cryosphere, thereby reducing its impact on the global shortwave energy budget by more than half, relative to the impact of pure snow. }}, doi = {10.1002/2017JE005368}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123..780S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRA..123.2441C, author = {{Chaufray}, J.-Y. and {Yelle}, R.~V. and {Gonzalez-Galindo}, F. and {Forget}, F. and {Lopez-Valverde}, M. and {Leblanc}, F. and {Modolo}, R.}, title = {{Effect of the Lateral Exospheric Transport on the Horizontal Hydrogen Distribution Near the Exobase of Mars}}, journal = {Journal of Geophysical Research (Space Physics)}, keywords = {Mars, exosphere, hydrogen}, year = 2018, volume = 123, pages = {2441-2454}, abstract = {{We simulate the hydrogen density near the exobase of Mars, using the 3-D Martian Global Circulation Model of Laboratoire de Météorologie Dynamique, coupled to an exospheric ballistic model to compute the downward ballistic flux. The simulated hydrogen distribution near the exobase obtained at two different seasons{\mdash}Ls = 180{\deg} and Ls = 270{\deg}{\mdash}is close to Zero Net Ballistic Flux equilibrium. In other words, the hydrogen density near the exobase adjusts to have a balance between the local upward ballistic and the downward ballistic flux due to a short lateral migration time in the exosphere compared to the vertical diffusion time. This equilibrium leads to a hydrogen density n near the exobase directly controlled by the exospheric temperature T by the relation nT^{5/2} = constant. This relation could be used to extend 1-D hydrogen exospheric model of Mars used to derive the hydrogen density and escape flux at Mars from Lyman-{\alpha} observations to 3-D model based on observed or modeled exospheric temperature near the exobase, without increasing the number of free parameters. }}, doi = {10.1002/2017JA025163}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRA..123.2441C}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018SSRv..214....7K, author = {{Korablev}, O. and {Montmessin}, F. and {Trokhimovskiy}, A. and {Fedorova}, A.~A. and {Shakun}, A.~V. and {Grigoriev}, A.~V. and {Moshkin}, B.~E. and {Ignatiev}, N.~I. and {Forget}, F. and {Lefèvre}, F. and {Anufreychik}, K. and {Dzuban}, I. and {Ivanov}, Y.~S. and {Kalinnikov}, Y.~K. and {Kozlova}, T.~O. and {Kungurov}, A. and {Makarov}, V. and {Martynovich}, F. and {Maslov}, I. and {Merzlyakov}, D. and {Moiseev}, P.~P. and {Nikolskiy}, Y. and {Patrakeev}, A. and {Patsaev}, D. and {Santos-Skripko}, A. and {Sazonov}, O. and {Semena}, N. and {Semenov}, A. and {Shashkin}, V. and {Sidorov}, A. and {Stepanov}, A.~V. and {Stupin}, I. and {Timonin}, D. and {Titov}, A.~Y. and {Viktorov}, A. and {Zharkov}, A. and {Altieri}, F. and {Arnold}, G. and {Belyaev}, D.~A. and {Bertaux}, J.~L. and {Betsis}, D.~S. and {Duxbury}, N. and {Encrenaz}, T. and {Fouchet}, T. and {Gérard}, J.-C. and {Grassi}, D. and {Guerlet}, S. and {Hartogh}, P. and {Kasaba}, Y. and {Khatuntsev}, I. and {Krasnopolsky}, V.~A. and {Kuzmin}, R.~O. and {Lellouch}, E. and {Lopez-Valverde}, M.~A. and {Luginin}, M. and {M{\"a}{\"a}tt{\"a}nen}, A. and {Marcq}, E. and {Martin Torres}, J. and {Medvedev}, A.~S. and {Millour}, E. and {Olsen}, K.~S. and {Patel}, M.~R. and {Quantin-Nataf}, C. and {Rodin}, A.~V. and {Shematovich}, V.~I. and {Thomas}, I. and {Thomas}, N. and {Vazquez}, L. and {Vincendon}, M. and {Wilquet}, V. and {Wilson}, C.~F. and {Zasova}, L.~V. and {Zelenyi}, L.~M. and {Zorzano}, M.~P.}, title = {{The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter}}, journal = {\ssr}, keywords = {Mars, Atmosphere, High-resolution spectrometer, Fourier-spectrometer, Echelle, Cross-dispersion}, year = 2018, volume = 214, eid = {7}, pages = {7}, abstract = {{The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (\gt10,000) and large spectral coverage (0.7 to 17 {\mu}m{\mdash}the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7-1.6 {\mu}m spectral range with a resolving power of {\tilde}20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2-4.4 {\mu}m range. MIR achieves a resolving power of \gt50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7-17 {\mu}m with apodized resolution varying from 0.2 to 1.3 cm^{-1}. TIRVIM is primarily dedicated to profiling temperature from the surface up to {\tilde}60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described. }}, doi = {10.1007/s11214-017-0437-6}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018SSRv..214....7K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..301..132C, author = {{Chaufray}, J.-Y. and {Gonzalez-Galindo}, F. and {Forget}, F. and {Lopez-Valverde}, M. and {Leblanc}, F. and {Modolo}, R. and {Hess}, S.}, title = {{Reply to comment On the hydrogen escape: Comment to variability of the hydrogen in the Martian upper atmosphere as simulated by a 3D atmosphere-exosphere coupling by J.-Y. Chaufray et al.'' by V. Krasnopolsky, Icarus, 281, 262}}, journal = {\icarus}, year = 2018, volume = 301, pages = {132-135}, abstract = {{Krasnopolsky (2017) makes a careful review of our recent results about the Martian hydrogen content of the Martian upper atmosphere (Chaufray et al., 2015). We comment here on his two major points. First, he suggests that the non-thermal escape of H_{2}, and particularly collisions with hot oxygen, not taken into account in our general circulation model (GCM), should modify our reported H_{2} and H density profiles. This is an important issue; we acknowledge that future effective coupling of our GCM with comprehensive models of the Martian solar wind interaction, ideally after being validated with the latest plasma observations of H_{2}^{+}$, would allow for better estimations of the relative importance of the H$_{2}$non-thermal and thermal escape processes. For the time being we need assumptions in the GCM, with proper and regular updates. According to a recent and detailed study of the anisotropic elastic and inelastic collision cross sections between O and H$_{2}$(Gacesa et al., 2012), the escape rates used by Krasnopolsky (2010) for this process might be overestimated. We therefore do not include non thermal escape of H$_{2}$in the model. And secondly, in response to Krasnopolsky's comment on the H escape variability with the solar cycle, we revised our calculations and found a small bug in the computation of the Jeans effusion velocity. Our revised computed H escape rates are included here. They have a small impact on our key conclusions: similar seasonal variations, a reduced variation with the solar cycle but still larger than Krasnopolsky (2017), and again a hydrogen scape systematically lower than the diffusion-limited flux. This bug does not affect the latest Mars Climate Database v5.2. }}, doi = {10.1016/j.icarus.2017.07.013}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..301..132C}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018P&SS..150...65E, author = {{Erard}, S. and {Cecconi}, B. and {Le Sidaner}, P. and {Rossi}, A.~P. and {Capria}, M.~T. and {Schmitt}, B. and {Génot}, V. and {André}, N. and {Vandaele}, A.~C. and {Scherf}, M. and {Hueso}, R. and {M{\"a}{\"a}tt{\"a}nen}, A. and {Thuillot}, W. and {Carry}, B. and {Achilleos}, N. and {Marmo}, C. and {Santolik}, O. and {Benson}, K. and {Fernique}, P. and {Beigbeder}, L. and {Millour}, E. and {Rousseau}, B. and {Andrieu}, F. and {Chauvin}, C. and {Minin}, M. and {Ivanoski}, S. and {Longobardo}, A. and {Bollard}, P. and {Albert}, D. and {Gangloff}, M. and {Jourdane}, N. and {Bouchemit}, M. and {Glorian}, J.-M. and {Trompet}, L. and {Al-Ubaidi}, T. and {Juaristi}, J. and {Desmars}, J. and {Guio}, P. and {Delaa}, O. and {Lagain}, A. and {Soucek}, J. and {Pisa}, D.}, title = {{VESPA: A community-driven Virtual Observatory in Planetary Science}}, journal = {\planss}, archiveprefix = {arXiv}, eprint = {1705.09727}, primaryclass = {astro-ph.IM}, keywords = {Virtual Observatory, Solar System, GIS}, year = 2018, volume = 150, pages = {65-85}, abstract = {{The VESPA data access system focuses on applying Virtual Observatory (VO) standards and tools to Planetary Science. Building on a previous EC-funded Europlanet program, it has reached maturity during the first year of a new Europlanet 2020 program (started in 2015 for 4 years). The infrastructure has been upgraded to handle many fields of Solar System studies, with a focus both on users and data providers. This paper describes the broad lines of the current VESPA infrastructure as seen by a potential user, and provides examples of real use cases in several thematic areas. These use cases are also intended to identify hints for future developments and adaptations of VO tools to Planetary Science. }}, doi = {10.1016/j.pss.2017.05.013}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018P%26SS..150...65E}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018JGRE..123..246G, author = {{Guerlet}, S. and {Fouchet}, T. and {Spiga}, A. and {Flasar}, F.~M. and {Fletcher}, L.~N. and {Hesman}, B.~E. and {Gorius}, N.}, title = {{Equatorial Oscillation and Planetary Wave Activity in Saturn's Stratosphere Through the Cassini Epoch}}, journal = {Journal of Geophysical Research (Planets)}, keywords = {Saturn, Cassini, atmosphere, infrared remote sensing, stratospheric dynamics}, year = 2018, volume = 123, pages = {246-261}, abstract = {{Thermal infrared spectra acquired by Cassini/Composite InfraRed Spectrometer (CIRS) in limb-viewing geometry in 2015 are used to derive 2-D latitude-pressure temperature and thermal wind maps. These maps are used to study the vertical structure and evolution of Saturn's equatorial oscillation (SEO), a dynamical phenomenon presenting similarities with the Earth's quasi-biennal oscillation (QBO) and semi-annual oscillation (SAO). We report that a new local wind maximum has appeared in 2015 in the upper stratosphere and derive the descent rates of other wind extrema through time. The phase of the oscillation observed in 2015, as compared to 2005 and 2010, remains consistent with a {\tilde}15 year period. The SEO does not propagate downward at a regular rate but exhibits faster descent rate in the upper stratosphere, combined with a greater vertical wind shear, compared to the lower stratosphere. Within the framework of a QBO-type oscillation, we estimate the absorbed wave momentum flux in the stratosphere to be on the order of {\tilde}7 {\times} 10$^{-6}$N m$^{-2}$. On Earth, interactions between vertically propagating waves (both planetary and mesoscale) and the mean zonal flow drive the QBO and SAO. To broaden our knowledge on waves potentially driving Saturn's equatorial oscillation, we searched for thermal signatures of planetary waves in the tropical stratosphere using CIRS nadir spectra. Temperature anomalies of amplitude 1-4 K and zonal wave numbers 1 to 9 are frequently observed, and an equatorial Rossby (n = 1) wave of zonal wave number 3 is tentatively identified in November 2009. }}, doi = {10.1002/2017JE005419}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123..246G}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018Icar..300..129M, author = {{Moore}, J.~M. and {Howard}, A.~D. and {Umurhan}, O.~M. and {White}, O.~L. and {Schenk}, P.~M. and {Beyer}, R.~A. and {McKinnon}, W.~B. and {Spencer}, J.~R. and {Singer}, K.~N. and {Grundy}, W.~M. and {Earle}, A.~M. and {Schmitt}, B. and {Protopapa}, S. and {Nimmo}, F. and {Cruikshank}, D.~P. and {Hinson}, D.~P. and {Young}, L.~A. and {Stern}, S.~A. and {Weaver}, H.~A. and {Olkin}, C.~B. and {Ennico}, K. and {Collins}, G. and {Bertrand}, T. and {Forget}, F. and {Scipioni}, F. and {New Horizons Science Team}}, title = {{Bladed Terrain on Pluto: Possible origins and evolution}}, journal = {\icarus}, keywords = {Pluto, Atmosphere, Ices, Mechanical properties, Geological processes, IR spectroscopy, Surface}, year = 2018, volume = 300, pages = {129-144}, abstract = {{Bladed Terrain on Pluto consists of deposits of massive CH$_{4}$, which are observed to occur within latitudes 30{\deg} of the equator and are found almost exclusively at the highest elevations ($\gt$2 km above the mean radius). Our analysis indicates that these deposits of CH$_{4}$preferentially precipitate at low latitudes where net annual solar energy input is lowest. CH$_{4}$and N$_{2}$will both precipitate at low elevations. However, since there is much more N$_{2}$in the atmosphere than CH$_{4}$, the N$_{2}$ice will dominate at these low elevations. At high elevations the atmosphere is too warm for N$_{2}$to precipitate so only CH$_{4}$can do so. We conclude that following the time of massive CH$_{4}$emplacement; there have been sufficient excursions in Pluto's climate to partially erode these deposits via sublimation into the blades we see today. Blades composed of massive CH$_{4}$ice implies that the mechanical behavior of CH$_{4}$can support at least several hundred meters of relief at Pluto surface conditions. Bladed Terrain deposits may be widespread in the low latitudes of the poorly seen sub-Charon hemisphere, based on spectral observations. If these locations are indeed Bladed Terrain deposits, they may mark heretofore unrecognized regions of high elevation. }}, doi = {10.1016/j.icarus.2017.08.031}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..300..129M}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }  @article{2018A&A...609A..64S, author = {{Sylvestre}, M. and {Teanby}, N.~A. and {Vinatier}, S. and {Lebonnois}, S. and {Irwin}, P.~G.~J.}, title = {{Seasonal evolution of C$_{2}$N$_{2}$, C$_{3}$H$_{4}$, and C$_{4}$H$_{2}$abundances in Titan's lower stratosphere}}, journal = {\aap}, archiveprefix = {arXiv}, eprint = {1709.09979}, primaryclass = {astro-ph.EP}, keywords = {planets and satellites: atmospheres, methods: data analysis}, year = 2018, volume = 609, eid = {A64}, pages = {A64}, abstract = {{ Aims: We study the seasonal evolution of Titan's lower stratosphere (around 15 mbar) in order to better understand the atmospheric dynamics and chemistry in this part of the atmosphere. Methods: We analysed Cassini/CIRS far-IR observations from 2006 to 2016 in order to measure the seasonal variations of three photochemical by-products: C$_{4}$H$_{2}$, C$_{3}$H$_{4}$, and C$_{2}$N$_{2}$. Results: We show that the abundances of these three gases have evolved significantly at northern and southern high latitudes since 2006. We measure a sudden and steep increase of the volume mixing ratios of C$_{4}$H$_{2}$, C$_{3}$H$_{4}$, and C$_{2}$N$_{2}$at the south pole from 2012 to 2013, whereas the abundances of these gases remained approximately constant at the north pole over the same period. At northern mid-latitudes, C$_{2}$N$_{2}$and C$_{4}$H$_{2}$abundances decrease after 2012 while C$_{3}$H$_{4}\$ abundances stay constant. The comparison of
these volume mixing ratio variations with the predictions of
photochemical and dynamical models provides constraints on the seasonal
evolution of atmospheric circulation and chemical processes at play.
}},
doi = {10.1051/0004-6361/201630255},