@comment{{This file has been generated by bib2bib 1.94}}
@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c year=2019 -c $type="ARTICLE" -oc pub2019.txt -ob pub2019.bib}}
  author = {{Turbet}, M. and {Tran}, H. and {Pirali}, O. and {Forget}, F. and 
	{Boulet}, C. and {Hartmann}, J.-M.},
  title = {{Far infrared measurements of absorptions by CH$_{4}$ + CO$_{2}$ and H$_{2}$ + CO$_{2}$ mixtures and implications for greenhouse warming on early Mars}},
  journal = {\icarus},
  archiveprefix = {arXiv},
  eprint = {1805.02595},
  primaryclass = {astro-ph.EP},
  keywords = {Mars, Spectroscopy, Measurement, Methane, Hydrogen, Collision induced absorptions, Climate},
  year = 2019,
  volume = 321,
  pages = {189-199},
  abstract = {{We present an experimental study of the absorption, between 40 and 640
cm$^{-1}$, by CO$_{2}$, CH$_{4}$ and H$_{2}$
gases as well as by H$_{2}$ + CO$_{2}$ and CH$_{4}$ +
CO$_{2}$ mixtures at room temperature. A Fourier transform
spectrometer associated to a multi-pass cell, whose optics were adjusted
to obtain a 152 m path length, were used to record transmission spectra
at total pressures up to about 0.98 bar. These measurements provide
information concerning the collision-induced absorption (CIA) bands as
well as about the wing of the CO$_{2}$ 15 {$\mu$}m band. Our results
for the CIAs of pure gases are, within uncertainties, in agreement with
previous determinations, validating our experimental and data analysis
procedures. We then consider the CIAs by H$_{2}$ + CO$_{2}$
and CH$_{4}$ + CO$_{2}$ and the low frequency wing of the
pure CO$_{2}$ 15 {$\mu$}m band, for which there are, to our
knowledge, no previous measurements. We confirm experimentally the
theoretical prediction of Wordsworth et al. (2017) that the
H$_{2}$ + CO$_{2}$ and CH$_{4}$ + CO$_{2}$ CIAs
are significantly stronger in the 50-550 cm$^{-1}$ region than
those of H$_{2}$ + N$_{2}$ and CH$_{4}$ +
N$_{2}$, respectively. However, we find that the shape and the
strength of these recorded CIAs differ from the aforementioned
predictions. For the pure CO$_{2}$ line-wings, we show that both
the {$\chi$}-factor deduced from measurements near 4 {$\mu$}m and a
line-mixing model very well describe the observed strongly
sub-Lorentzian behavior in the 500-600 cm$^{-1}$ region. These
experimental results open renewed perspectives for studies of the past
climate of Mars and extrasolar analogues.
  doi = {10.1016/j.icarus.2018.11.021},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Encrenaz}, T. and {Greathouse}, T.~K. and {Marcq}, E. and {Sagawa}, H. and 
	{Widemann}, T. and {Bézard}, B. and {Fouchet}, T. and {Lefèvre}, F. and 
	{Lebonnois}, S. and {Atreya}, S.~K. and {Lee}, Y.~J. and {Giles}, R. and 
	{Watanabe}, S.},
  title = {{HDO and SO$_{2}$ thermal mapping on Venus. IV. Statistical analysis of the SO$_{2}$ plumes}},
  journal = {\aap},
  keywords = {planets and satellites: atmospheres, planets and satellites: terrestrial planets, infrared: planetary systems},
  year = 2019,
  volume = 623,
  eid = {A70},
  pages = {A70},
  abstract = {{Since January 2012 we have been monitoring the behavior of sulfur
dioxide and water on Venus, using the Texas Echelon Cross-Echelle
Spectrograph (TEXES) imaging spectrometer at the NASA InfraRed Telescope
Facility (IRTF, Mauna Kea Observatory). We present here the observations
obtained between January 2016 and September 2018. As in the case of our
previous runs, data were recorded around 1345 cm$^{-1}$ (7.4
{$\mu$}m). The molecules SO$_{2}$, CO$_{2}$, and HDO (used as a
proxy for H$_{2}$O) were observed, and the cloudtop of Venus was
probed at an altitude of about 64 km. The volume mixing ratio of
SO$_{2}$ was estimated using the SO$_{2}$/CO$_{2}$
line depth ratios of weak transitions; the H$_{2}$O volume mixing
ratio was derived from the HDO/CO$_{2}$ line depth ratio, assuming
a D/H ratio of 200 times the Vienna Standard Mean Ocean Water (VSMOW).
As reported in our previous analyses, the SO$_{2}$ mixing ratio
shows strong variations with time and also over the disk, showing
evidence of the formation of SO$_{2}$ plumes with a lifetime of a
few hours; in contrast, the H$_{2}$O abundance is remarkably
uniform over the disk and shows moderate variations as a function of
time. We performed a statistical analysis of the behavior of the
SO$_{2}$ plumes, using all TEXES data between 2012 and 2018. They
appear mostly located around the equator. Their distribution as a
function of local time seems to show a depletion around noon; we do not
have enough data to confirm this feature definitely. The distribution of
SO$_{2}$ plumes as a function of longitude shows no clear feature,
apart from a possible depletion around 100E-150E and around 300E-360E.
There seems to be a tendency for the H$_{2}$O volume mixing ratio
to decrease after 2016, and for the SO$_{2}$ mixing ratio to
increase after 2014. However, we see no clear anti-correlation between
the SO$_{2}$ and H$_{2}$O abundances at the cloudtop,
neither on the individual maps nor over the long term. Finally, there is
a good agreement between the TEXES results and those obtained in the UV
range (SPICAV/Venus Express and UVI/Akatsuki) at a slightly higher
altitude. This agreement shows that SO$_{2}$ observations obtained
in the thermal infrared can be used to extend the local time coverage of
the SO$_{2}$ measurements obtained in the UV range.
  doi = {10.1051/0004-6361/201833511},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Nishikawa}, Y. and {Lognonné}, P. and {Kawamura}, T. and 
	{Spiga}, A. and {Stutzmann}, E. and {Schimmel}, M. and {Bertrand}, T. and 
	{Forget}, F. and {Kurita}, K.},
  title = {{Mars' Background Free Oscillations}},
  journal = {\ssr},
  keywords = {Mars, Planetary free oscillation, GCM, Seismometer, Normal mode, InSight},
  year = 2019,
  volume = 215,
  eid = {13},
  pages = {13},
  abstract = {{Observations and inversion of the eigenfrequencies of free oscillations
constitute powerful tools to investigate the internal structure of a
planet. On Mars, such free oscillations can be excited by atmospheric
pressure and wind stresses from the Martian atmosphere, analogous to
what occurs on Earth. Over long periods and on a global scale, this
phenomenon may continuously excite Mars' background free oscillations
(MBFs), which constitute the so-called Martian hum. However, the source
exciting MBFs is related both to the global-scale atmospheric
circulation on Mars and to the variations in pressure and wind at the
planetary boundary layer, for which no data are available.

To overcome this drawback, we focus herein on a global-scale source and
use results of simulations based on General Circular Models (GCMs). GCMs
can predict and reproduce long-term, global-scale Martian pressure and
wind variations and suggest that, contrary to what happens on Earth,
daily correlations in the Martian hum might be generated by the
solar-driven GCM. After recalling the excitation terms, we calculate
MBFs by using GCM computations and estimate the contribution to the hum
made by the global atmospheric circulation. Although we work at the
lower limit of MBF signals, the results indicate that the signal is
likely to be periodic, which would allow us to use more efficient
stacking theories than can be applied to Earth's hum. We conclude by
discussing the perspectives for the InSight SEIS instrument to detect
the Martian hum. The amplitude of the MBF signal is on the order of
nanogals and is therefore hidden by instrumental and thermal noise,
which implies that, provided the predicted daily coherence in hum
excitation is present, the InSight SEIS seismometer should be capable of
  doi = {10.1007/s11214-019-0579-9},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Ferri}, F. and {Karatekin}, {\"O}. and {Lewis}, S.~R. and {Forget}, F. and 
	{Aboudan}, A. and {Colombatti}, G. and {Bettanini}, C. and {Debei}, S. and 
	{Van Hove}, B. and {Dehant}, V. and {Harri}, A.-M. and {Leese}, M. and 
	{M{\"a}kinen}, T. and {Millour}, E. and {Muller-Wodarg}, I. and 
	{Ori}, G.~G. and {Pacifici}, A. and {Paris}, S. and {Patel}, M. and 
	{Schoenenberger}, M. and {Herath}, J. and {Siili}, T. and {Spiga}, A. and 
	{Tokano}, T. and {Towner}, M. and {Withers}, P. and {Asmar}, S. and 
	{Plettemeier}, D.},
  title = {{ExoMars Atmospheric Mars Entry and Landing Investigations and Analysis (AMELIA)}},
  journal = {\ssr},
  keywords = {Mars, Entry Descent and Landing (EDL), Dynamical models, Trajectory, Attitude, Atmospheric investigations},
  year = 2019,
  volume = 215,
  eid = {8},
  pages = {8},
  abstract = {{The entry, descent and landing of Schiaparelli, the ExoMars Entry,
descent and landing Demonstrator Module (EDM), offered a rare
(once-per-mission) opportunity for in situ investigations of the martian
environment over a wide altitude range. The aim of the ExoMars AMELIA
experiment was to exploit the Entry, Descent and Landing System (EDLS)
engineering measurements for scientific investigations of Mars'
atmosphere and surface. Here we present the simulations, modelling and
the planned investigations prior to the Entry, Descent and Landing (EDL)
event that took place on 19th October 2016. Despite the unfortunate
conclusion of the Schiaparelli mission, flight data recorded during the
entry and the descent until the loss of signal, have been recovered.
These flight data, although limited and affected by transmission
interruptions and malfunctions, are essential for investigating the
anomaly and validating the EDL operation, but can also contribute
towards the partial achievement of AMELIA science objectives.
  doi = {10.1007/s11214-019-0578-x},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{White}, O.~L. and {Moore}, J.~M. and {Howard}, A.~D. and {McKinnon}, W.~B. and 
	{Keane}, J.~T. and {Singer}, K.~N. and {Bertrand}, T. and {Robbins}, S.~J. and 
	{Schenk}, P.~M. and {Schmitt}, B. and {Buratti}, B.~J. and {Stern}, S.~A. and 
	{Ennico}, K. and {Olkin}, C.~B. and {Weaver}, H.~A. and {Young}, L.~A. and 
	{New Horizons Geology}, G. and {Imaging Theme Team}},
  title = {{Washboard and fluted terrains on Pluto as evidence for ancient glaciation}},
  journal = {Nature Astronomy},
  year = 2019,
  volume = 3,
  pages = {62-68},
  abstract = {{Distinctive landscapes termed `washboard' and `fluted'
terrains$^{1,2}$, which border the N$_{2}$ ice plains of
Sputnik Planitia along its northwest margin, are among the most
enigmatic landforms yet seen on Pluto. These terrains consist of
parallel to sub-parallel ridges that display a remarkably consistent
east-northeast-west-southwest orientation{\mdash}a configuration that
does not readily point to a simple analogous terrestrial or planetary
process or landform. Here, we report on mapping and analysis of their
morphometry and distribution as a means to determine their origin. Based
on their occurrence in generally low-elevation, low-relief settings
adjacent to Sputnik Planitia that coincide with a major tectonic system,
and through comparison with fields of sublimation pits seen in southern
Sputnik Planitia, we conclude that washboard and fluted terrains
represent crustal debris that were buoyant in pitted glacial
N$_{2}$ ice that formerly covered this area, and which were
deposited after the N$_{2}$ ice receded via sublimation. Crater
surface age estimates indicate that this N$_{2}$ ice glaciation
formed and disappeared early in Pluto's history, soon after formation of
the Sputnik Planitia basin. These terrains constitute an entirely new
category of glacial landform.
  doi = {10.1038/s41550-018-0592-z},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Ordonez-Etxeberria}, I. and {Hueso}, R. and {S{\'a}nchez-Lavega}, A. and 
	{Millour}, E. and {Forget}, F.},
  title = {{Meteorological pressure at Gale crater from a comparison of REMS/MSL data and MCD modelling: Effect of dust storms}},
  journal = {\icarus},
  keywords = {Mars, atmosphere, Mars, climate, Atmospheres, dynamics, Dust storms},
  year = 2019,
  volume = 317,
  pages = {591-609},
  abstract = {{We examine the record of atmospheric pressure in Gale crater measured
in-situ by the Rover Environmental Monitoring Station (REMS) instrument
(G{\'o}mez-Elvira et al., 2012) on the Mars Science Laboratory (MSL)
rover over two Martian years. We compare the data with pressure
predictions from the Mars Climate Database (MCD) (Forget et al., 1999;
Millour et al., 2015) version 5.2, which is a climatological database
derived from numerical simulations of the Martian atmosphere produced by
a General Circulation Model run over several Martian years. Seasonal and
daily trends in pressure data from REMS are well reproduced by the
standard climatology of the MCD using its high resolution mode. This
high-resolution mode extrapolates pressure values from the nominal model
into the altitude of each location using a high-resolution topography
model and a fine tuning of the vertical scale height that was chosen to
mimic effects of slope winds not directly accounted for in the General
Circulation Model on which the MCD is based. Differences between the
synthetic MCD pressure data and the REMS measurements are produced by
meteorological features that are identified on particular groups of sols
and quantified in intensity. We show that regional dust storms outside
Gale crater and dust abundance at the crater are important factors in
the behaviour of the pressure exciting larger amplitudes on the daily
pressure variations and causing most of the largest REMS-MCD
differences. We compare the pressure signals with published data of the
dust optical depth obtained by the REMS ultraviolet photodiodes and the
Mastcam instrument on MSL, and with orbital images of the planet
acquired by the MARCI instrument on the Mars Reconnaissance Orbiter
(MRO). We show that in some cases regional dust storms induce a
characteristic signature in the surface pressure measured by REMS
several sols before the dust arrives to Gale crater. We explore the
capability of daily pressure measurements to serve as a fast detector of
the development of dust storms in the context of the MSL, Insight and
Mars 2020 missions.
  doi = {10.1016/j.icarus.2018.09.003},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Pluriel}, W. and {Marcq}, E. and {Turbet}, M.},
  title = {{Modeling the albedo of Earth-like magma ocean planets with H$_{2}$O-CO$_{2}$ atmospheres}},
  journal = {\icarus},
  archiveprefix = {arXiv},
  eprint = {1809.02036},
  primaryclass = {astro-ph.EP},
  keywords = {Atmospheres, Albedo, Spectroscopy, Radiative transfer, Modeling},
  year = 2019,
  volume = 317,
  pages = {583-590},
  abstract = {{During accretion, the young rocky planets are so hot that they become
endowed with a magma ocean. From that moment, the mantle convective
thermal flux control the cooling of the planet and an atmosphere is
created by outgassing. This atmosphere will then play a key role during
this cooling phase. Studying this cooling phase in details is a
necessary step to explain the great diversity of the observed telluric
planets and especially to assess the presence of surface liquid water.
We used here a radiative-convective 1D atmospheric model
(H$_{2}$O, CO$_{2}$) to study the impact of the Bond albedo
on the evolution of magma ocean planets. We derived from this model the
thermal emission spectrum and the spectral reflectance of these planets,
from which we calculated their Bond albedos. Compared to Marcq et al.
(2017), the model now includes a new module to compute the Rayleigh
scattering, and state of the art CO$_{2}$ and H$_{2}$O
gaseous opacities data in the visible and infrared spectral ranges. We
show that the Bond albedo of these planets depends on their surface
temperature and results from a competition between Rayleigh scattering
from the gases and Mie scattering from the clouds. The colder the
surface temperature is, the thicker the clouds are, and the higher the
Bond albedo is. We also evidence that the relative abundances of
CO$_{2}$ and H$_{2}$O in the atmosphere strongly impact the
Bond albedo. The Bond albedo is higher for atmospheres dominated by the
CO$_{2}$, better Rayleigh scatterer than H$_{2}$O. Finally,
we provide the community with an empirical formula for the Bond albedo
that could be useful for future studies of magma ocean planets.
  doi = {10.1016/j.icarus.2018.08.023},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}