pub2019.bib

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@article{2019Icar..321..189T,
  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 = {http://adsabs.harvard.edu/abs/2019Icar..321..189T},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2019Icar..317..591O,
  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 = {http://adsabs.harvard.edu/abs/2019Icar..317..591O},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2019Icar..317..583P,
  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 = {http://adsabs.harvard.edu/abs/2019Icar..317..583P},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}