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@comment{{This file has been generated by bib2bib 1.95}}
@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c 'not journal:"Polymer Science"' -c '  author:"Madeleine"  ' -c year=2012 -c $type="ARTICLE" -oc lmd_Madeleine2012.txt -ob lmd_Madeleine2012.bib /home/WWW/LMD/public/}}
  author = {{Madeleine}, J.-B. and {Forget}, F. and {Millour}, E. and {Navarro}, T. and 
	{Spiga}, A.},
  title = {{The influence of radiatively active water ice clouds on the Martian climate}},
  journal = {\grl},
  keywords = {Atmospheric Composition and Structure: Cloud/radiation interaction, Atmospheric Composition and Structure: Planetary atmospheres (5210, 5405, 5704), Atmospheric Processes: Clouds and cloud feedbacks, Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solar System Objects: Mars},
  year = 2012,
  month = dec,
  volume = 39,
  eid = {L23202},
  pages = {23202},
  abstract = {{Radiatively active water ice clouds (RAC) play a key role in shaping the
thermal structure of the Martian atmosphere. In this paper, RAC are
implemented in the LMD Mars Global Climate Model (GCM) and the simulated
temperatures are compared to Thermal Emission Spectrometer observations
over a full year. RAC change the temperature gradients and global
dynamics of the atmosphere and this change in dynamics in turn implies
large-scale adiabatic temperature changes. Therefore, clouds have both a
direct and indirect effect on atmospheric temperatures. RAC successfully
reduce major GCM temperature biases, especially in the regions of
formation of the aphelion cloud belt where a cold bias of more than 10 K
is corrected. Departures from the observations are however seen in the
polar regions, and highlight the need for better modeling of cloud
formation and evolution.
  doi = {10.1029/2012GL053564},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Clancy}, R.~T. and {Sandor}, B.~J. and {Wolff}, M.~J. and {Smith}, M.~D. and 
	{Lefèvre}, F. and {Madeleine}, J.-B. and {Forget}, F. and 
	{Murchie}, S.~L. and {Seelos}, F.~P. and {Seelos}, K.~D. and 
	{Nair}, H.~A. and {Toigo}, A.~D. and {Humm}, D. and {Kass}, D.~M. and 
	{Kleinb{\"o}hl}, A. and {Heavens}, N.},
  title = {{Extensive MRO CRISM observations of 1.27 {$\mu$}m O$_{2}$ airglow in Mars polar night and their comparison to MRO MCS temperature profiles and LMD GCM simulations}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Aurorae and airglow, Planetary Sciences: Solid Surface Planets: Polar regions, Planetary Sciences: Solid Surface Planets: Remote sensing, Planetary Sciences: Solar System Objects: Mars},
  year = 2012,
  month = aug,
  volume = 117,
  eid = {E00J10},
  pages = {0},
  abstract = {{The Martian polar night distribution of 1.27 {$\mu$}m (0-0) band
emission from O$_{2}$ singlet delta
[O$_{2}$($^{1}${$\Delta$}$_{g}$)] is determined from an
extensive set of Mars Reconnaissance Orbiter (MRO) Compact
Reconnaissance Imaging Spectral Mapping (CRISM) limb scans observed over
a wide range of Mars seasons, high latitudes, local times, and
longitudes between 2009 and 2011. This polar nightglow reflects
meridional transport and winter polar descent of atomic oxygen produced
from CO$_{2}$ photodissociation. A distinct peak in 1.27 {$\mu$}m
nightglow appears prominently over 70-90NS latitudes at
40-60 km altitudes, as retrieved for over 100 vertical profiles of
O$_{2}$($^{1}${$\Delta$}$_{g}$) 1.27 {$\mu$}m volume
emission rates (VER). We also present the first detection of much
({\times}80 {\plusmn} 20) weaker 1.58 {$\mu$}m (0-1) band emission from
Mars O$_{2}$($^{1}${$\Delta$}$_{g}$). Co-located polar
night CRISM O$_{2}$($^{1}${$\Delta$}$_{g}$) and Mars
Climate Sounder (MCS) (McCleese et al., 2008) temperature profiles are
compared to the same profiles as simulated by the Laboratoire de
Météorologie Dynamique (LMD) general
circulation/photochemical model (e.g., Lefèvre et al., 2004).
Both standard and interactive aerosol LMD simulations (Madeleine et al.,
2011a) underproduce CRISM O$_{2}$($^{1}${$\Delta$}$_{g}$)
total emission rates by 40\%, due to inadequate transport of atomic
oxygen to the winter polar emission regions. Incorporation of
interactive cloud radiative forcing on the global circulation leads to
distinct but insufficient improvements in modeled polar
O$_{2}$($^{1}${$\Delta$}$_{g}$) and temperatures. The
observed and modeled anti-correlations between temperatures and 1.27
{$\mu$}m band VER reflect the temperature dependence of the rate
coefficient for O$_{2}$($^{1}${$\Delta$}$_{g}$)
formation, as provided in Roble (1995).
  doi = {10.1029/2011JE004018},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Madeleine}, J.-B. and {Forget}, F. and {Spiga}, A. and {Wolff}, M.~J. and 
	{Montmessin}, F. and {Vincendon}, M. and {Jouglet}, D. and {Gondet}, B. and 
	{Bibring}, J.-P. and {Langevin}, Y. and {Schmitt}, B.},
  title = {{Aphelion water-ice cloud mapping and property retrieval using the OMEGA imaging spectrometer onboard Mars Express}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Atmospheric Composition and Structure: Planetary atmospheres (5210, 5405, 5704), Biogeosciences: Remote sensing, Mathematical Geophysics: Spectral analysis (3205, 3280, 4319), Atmospheric Processes: Clouds and aerosols, Planetary Sciences: Solar System Objects: Mars},
  year = 2012,
  month = may,
  volume = 117,
  eid = {E00J07},
  pages = {0},
  abstract = {{Mapping of the aphelion clouds over the Tharsis plateau and retrieval of
their particle size and visible opacity are made possible by the OMEGA
imaging spectrometer aboard Mars Express. Observations cover the period
from MY26 L$_{s}$ = 330{\deg} to MY29 L$_{s}$ = 180{\deg} and
are acquired at various local times, ranging from 8 AM to 6 PM. Cloud
maps of the Tharsis region constructed using the 3.1 {$\mu$}m ice
absorption band reveal the seasonal and diurnal evolution of aphelion
clouds. Four distinct types of clouds are identified: morning hazes,
topographically controlled hazes, cumulus clouds and thick hazes. The
location and time of occurrence of these clouds are analyzed and their
respective formation process is discussed. An inverse method for
retrieving cloud particle size and opacity is then developed and can
only be applied to thick hazes. The relative error of these measurements
is less than 30\% for cloud particle size and 20\% for opacity. Two groups
of particles can be distinguished. The first group is found over flat
plains and is composed of relatively small particles, ranging in size
from 2 to 3.5 {$\mu$}m. The second group is characterized by particle sizes
of {\tilde}5 {$\mu$}m which appear to be quite constant over L$_{s}$ and
local time. It is found west of Ascraeus and Pavonis Mons, and near
Lunae Planum. These regions are preferentially exposed to anabatic
winds, which may control the formation of these particles and explain
their distinct properties. The water ice column is equal to 2.9 pr.{$\mu$}m
on average, and can reach 5.2 pr.{$\mu$}m in the thickest clouds of
  doi = {10.1029/2011JE003940},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Kerber}, L. and {Head}, J.~W. and {Madeleine}, J.-B. and {Forget}, F. and 
	{Wilson}, L.},
  title = {{The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits}},
  journal = {\icarus},
  year = 2012,
  month = may,
  volume = 219,
  pages = {358-381},
  abstract = {{A number of voluminous, fine-grained, friable deposits have been mapped
on Mars. The modes of origin for these deposits are debated. The
feasibility for an origin by volcanic airfall for the friable deposits
is tested using a global circulation model to simulate the dispersal of
pyroclasts from candidate source volcanoes near each deposit. It is
concluded that the Medusae Fossae Formation and Electris deposits are
easily formed through volcanic processes, and that the Hellas deposits
and south polar pitted deposits could have some contribution from
volcanic sources in specific atmospheric regimes. The Arabia and Argyre
deposits are not well replicated by modeled pyroclast dispersal,
suggesting that these deposits were most likely emplaced by other means.
  doi = {10.1016/j.icarus.2012.03.016},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Fastook}, J.~L. and {Head}, J.~W. and {Marchant}, D.~R. and 
	{Forget}, F. and {Madeleine}, J.-B.},
  title = {{Early Mars climate near the Noachian-Hesperian boundary: Independent evidence for cold conditions from basal melting of the south polar ice sheet (Dorsa Argentea Formation) and implications for valley network formation}},
  journal = {\icarus},
  year = 2012,
  month = may,
  volume = 219,
  pages = {25-40},
  abstract = {{Currently, and throughout much of the Amazonian, the mean annual surface
temperatures of Mars are so cold that basal melting does not occur in
ice sheets and glaciers and they are cold-based. The documented evidence
for extensive and well-developed eskers (sediment-filled former
sub-glacial meltwater channels) in the south circumpolar Dorsa Argentea
Formation is an indication that basal melting and wet-based glaciation
occurred at the South Pole near the Noachian-Hesperian boundary. We
employ glacial accumulation and ice-flow models to distinguish between
basal melting from bottom-up heat sources (elevated geothermal fluxes)
and top-down induced basal melting (elevated atmospheric temperatures
warming the ice). We show that under mean annual south polar atmospheric
temperatures (-100 {\deg}C) simulated in typical Amazonian climate
experiments and typical Noachian-Hesperian geothermal heat fluxes (45-65
mW/m$^{2}$), south polar ice accumulations remain cold-based. In
order to produce significant basal melting with these typical geothermal
heat fluxes, the mean annual south polar atmospheric temperatures must
be raised from today's temperature at the surface (-100 {\deg}C) to the
range of -50 to -75 {\deg}C. This mean annual polar surface atmospheric
temperature range implies lower latitude mean annual temperatures that
are likely to be below the melting point of water, and thus does not
favor a ''warm and wet'' early Mars. Seasonal temperatures at lower
latitudes, however, could range above the melting point of water,
perhaps explaining the concurrent development of valley networks and
open basin lakes in these areas. This treatment provides an independent
estimate of the polar (and non-polar) surface temperatures near the
Noachian-Hesperian boundary of Mars history and implies a cold and
relatively dry Mars climate, similar to the Antarctic Dry Valleys, where
seasonal melting forms transient streams and permanent ice-covered lakes
in an otherwise hyperarid, hypothermal climate.
  doi = {10.1016/j.icarus.2012.02.013},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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