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@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c year=2018 -c $type="ARTICLE" -oc pub2018.txt -ob pub2018.bib}}
  author = {{Tran}, H. and {Turbet}, M. and {Chelin}, P. and {Landsheere}, X.
  title = {{Measurements and modeling of absorption by CO$_{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 = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  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
($\gt$10,000) and large spectral coverage (0.7 to 17 {$\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 $\gt$50,000. It has been designed to accomplish the most sensitive
measurements ever of the trace gases present in the Martian atmosphere.
The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum
Fourier-transform spectrometer encompassing the spectral range of 1.7-17
{$\mu$}m with apodized resolution varying from 0.2 to 1.3 cm$^{-1}$.
TIRVIM is primarily dedicated to profiling temperature from the surface
up to {\tilde}60 km and to monitor aerosol abundance in nadir. TIRVIM
also has a limb and solar occultation capability. The technical concept
of the instrument, its accommodation on the spacecraft, the optical
designs as well as some of the calibrations, and the expected
performances for its three channels are described.
  doi = {10.1007/s11214-017-0437-6},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Chaufray}, J.-Y. and {Gonzalez-Galindo}, F. and {Forget}, F. and 
	{Lopez-Valverde}, M. and {Leblanc}, F. and {Modolo}, R. and 
	{Hess}, S.},
  title = {{Reply to comment ``On the hydrogen escape: Comment to variability of the hydrogen in the Martian upper atmosphere as simulated by a 3D atmosphere-exosphere coupling by J.-Y. Chaufray et al.'' by V. Krasnopolsky, Icarus, 281, 262}},
  journal = {\icarus},
  year = 2018,
  volume = 301,
  pages = {132-135},
  abstract = {{Krasnopolsky (2017) makes a careful review of our recent results about
the Martian hydrogen content of the Martian upper atmosphere (Chaufray
et al., 2015). We comment here on his two major points. First, he
suggests that the non-thermal escape of H$_{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 = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  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 = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  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
  doi = {10.1016/j.icarus.2017.08.031},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  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},
  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}, adsurl = {}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }