lmd_Madeleine2011.bib

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@article{2011JGRE..11611010M,
  author = {{Madeleine}, J.-B. and {Forget}, F. and {Millour}, E. and {Montabone}, L. and 
	{Wolff}, M.~J.},
  title = {{Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Hydrology: Model calibration (3333), Atmospheric Processes: Clouds and aerosols, Atmospheric Processes: Global climate models (1626, 4928), Atmospheric Processes: Radiative processes, Planetary Sciences: Solar System Objects: Mars},
  year = 2011,
  month = nov,
  volume = 116,
  number = e15,
  eid = {E11010},
  pages = {11010},
  abstract = {{Airborne dust is the main driver of Martian atmospheric temperature, and
accurately accounting for its radiative effect in Global Climate Models
(GCMs) is essential. This requires the modeling of the dust distribution
and radiative properties, and when trying to simulate the true climate
variability, the use of the observed dust column opacity to guide the
model. A recurrent problem has been the inability of Mars GCMs to
predict realistic temperatures while using both the observed dust
radiative properties and column opacity. One would have to drive the
model with a tuned opacity to reach an agreement with the observations,
thereby losing its self-consistency. In this paper, we show that using
the most recently derived dust radiative properties in the LMD
(Laboratoire de Météorologie Dynamique) GCM solves this
problem, which was mainly due to the underestimation of the dust single
scattering albedo in the solar domain. However, an overall warm
temperature bias remains above the 1 hPa pressure level. We therefore
refine the model by implementing a {\ldquo}semi-interactive{\rdquo} dust
transport scheme which is coupled to the radiative transfer
calculations. This scheme allows a better representation of the dust
layer depth in the model and thereby removes the remaining warm bias.
The LMD/GCM is now able to predict accurate temperatures without any
tuning of the dust opacity used to guide the model. Remaining
discrepancies are discussed, and seem to be primarily due to the neglect
of the radiative effect of water-ice clouds, and secondarily to
persisting uncertainties in the dust spatial distribution.
}},
  doi = {10.1029/2011JE003855},
  adsurl = {http://adsabs.harvard.edu/abs/2011JGRE..11611010M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011Icar..216..212K,
  author = {{Kerber}, L. and {Head}, J.~W. and {Madeleine}, J.-B. and {Forget}, F. and 
	{Wilson}, L.},
  title = {{The dispersal of pyroclasts from Apollinaris Patera, Mars: Implications for the origin of the Medusae Fossae Formation}},
  journal = {\icarus},
  year = 2011,
  month = nov,
  volume = 216,
  pages = {212-220},
  abstract = {{The Medusae Fossae Formation (MFF) has long been thought to be of
Amazonian age, but recent studies propose that a significant part of its
emplacement occurred in the Hesperian and that many of the Amazonian
ages represent modification (erosional and redepositional) ages. On the
basis of the new formational age, we assess the hypothesis that
explosive eruptions from Apollinaris Patera might have been the source
of the Medusae Fossae Formation. In order to assess the likelihood of
this hypothesis, we examine stratigraphic relationships between
Apollinaris Patera and the MFF and analyze the relief of the MFF using
topographic data. We predict the areal distribution of tephra erupted
from Apollinaris Patera using a Mars Global Circulation Model (GCM)
combined with a semi-analytical explosive eruption model for Mars, and
compare this with the distribution of the MFF. We conclude that
Apollinaris Patera could have been responsible for the emplacement of
the Medusae Fossae Formation.
}},
  doi = {10.1016/j.icarus.2011.07.035},
  adsurl = {http://adsabs.harvard.edu/abs/2011Icar..216..212K},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011Icar..216...23F,
  author = {{Fastook}, J.~L. and {Head}, J.~W. and {Forget}, F. and {Madeleine}, J.-B. and 
	{Marchant}, D.~R.},
  title = {{Evidence for Amazonian northern mid-latitude regional glacial landsystems on Mars: Glacial flow models using GCM-driven climate results and comparisons to geological observations}},
  journal = {\icarus},
  year = 2011,
  month = nov,
  volume = 216,
  pages = {23-39},
  abstract = {{A fretted valley system on Mars located at the northern mid-latitude
dichotomy boundary contains lineated valley fill (LVF) with extensive
flow-like features interpreted to be glacial in origin. We have modeled
this deposit using glacial flow models linked to atmospheric general
circulation models (GCM) for conditions consistent with the deposition
of snow and ice in amounts sufficient to explain the interpreted
glaciation. In the first glacial flow model simulation, sources were
modeled in the alcoves only and were found to be consistent with the
alpine valley glaciation interpretation for various environments of flow
in the system. These results supported the interpretation of the
observed LVF deposits as resulting from initial ice accumulation in the
alcoves, accompanied by debris cover that led to advancing alpine
glacial landsystems to the extent observed today, with preservation of
their flow texture and the underlying ice during downwasting in the
waning stages of glaciation. In the second glacial flow model
simulation, the regional accumulation patterns predicted by a GCM linked
to simulation of a glacial period were used. This glacial flow model
simulation produced a much wider region of thick ice accumulation, and
significant glaciation on the plateaus and in the regional plains
surrounding the dichotomy boundary. Deglaciation produced decreasing ice
thicknesses, with flow centered on the fretted valleys. As plateaus lost
ice, scarps and cliffs of the valley and dichotomy boundary walls were
exposed, providing considerable potential for the production of a rock
debris cover that could preserve the underlying ice and the surface flow
patterns seen today. In this model, the lineated valley fill and lobate
debris aprons were the product of final retreat and downwasting of a
much larger, regional glacial landsystem, rather than representing the
maximum extent of an alpine valley glacial landsystem. These results
favor the interpretation that periods of mid-latitude glaciation were
characterized by extensive plateau and plains ice cover, rather than
being restricted to alcoves and adjacent valleys, and that the observed
lineated valley fill and lobate debris aprons represent debris-covered
residual remnants of a once more extensive glaciation.
}},
  doi = {10.1016/j.icarus.2011.07.018},
  adsurl = {http://adsabs.harvard.edu/abs/2011Icar..216...23F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011ApJ...733L..48W,
  author = {{Wordsworth}, R.~D. and {Forget}, F. and {Selsis}, F. and {Millour}, E. and 
	{Charnay}, B. and {Madeleine}, J.-B.},
  title = {{Gliese 581d is the First Discovered Terrestrial-mass Exoplanet in the Habitable Zone}},
  journal = {\apjl},
  archiveprefix = {arXiv},
  eprint = {1105.1031},
  primaryclass = {astro-ph.EP},
  keywords = {astrobiology, planets and satellites: atmospheres, planet-star interactions, techniques: spectroscopic},
  year = 2011,
  month = jun,
  volume = 733,
  eid = {L48},
  pages = {L48},
  abstract = {{It has been suggested that the recently discovered exoplanet GJ581d
might be able to support liquid water due to its relatively low mass and
orbital distance. However, GJ581d receives 35\% less stellar energy than
Mars and is probably locked in tidal resonance, with extremely low
insolation at the poles and possibly a permanent night side. Under such
conditions, it is unknown whether any habitable climate on the planet
would be able to withstand global glaciation and/or atmospheric
collapse. Here we present three-dimensional climate simulations which
demonstrate that GJ581d will have a stable atmosphere and surface liquid
water for a wide range of plausible cases, making it the first confirmed
super-Earth (exoplanet of 2-10 Earth masses) in the habitable zone. We
find that atmospheres with over 10 bar CO$_{2}$ and varying
amounts of background gas (e.g., N$_{2}$) yield global mean
temperatures above 0{\deg}C for both land and ocean-covered surfaces.
Based on the emitted IR radiation calculated by the model, we propose
observational tests that will allow these cases to be distinguished from
other possible scenarios in the future.
}},
  doi = {10.1088/2041-8205/733/2/L48},
  adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...733L..48W},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011Icar..213..131P,
  author = {{Pilorget}, C. and {Forget}, F. and {Millour}, E. and {Vincendon}, M. and 
	{Madeleine}, J.~B.},
  title = {{Dark spots and cold jets in the polar regions of Mars: New clues from a thermal model of surface CO $_{2}$ ice}},
  journal = {\icarus},
  year = 2011,
  month = may,
  volume = 213,
  pages = {131-149},
  abstract = {{Observations of the martian CO $_{2}$ ice cap in late winter and
spring have revealed exotic phenomena. Unusual dark spots, fans and
blotches form as the south-polar seasonal CO $_{2}$ ice cap
retreats. The formation mechanisms of these features are not clearly
understood. Theoretical models suggest that photons could penetrate deep
into the CO $_{2}$ ice down to the regolith, leading to basal
sublimation and gas and dust ejection. We have developed a detailed
thermal model able to simulate the temporal evolution of the regolith-CO
$_{2}$ ice layer-atmosphere column. It takes into account heat
conduction, radiative transfer within the ice and the atmosphere, and
latent heat exchange when there is a phase transition. We found that a
specific algorithm, fully coupling these three components, was needed to
properly predict ice sublimation below the surface. Our model allows us
to determine under what conditions basal sublimation is possible and
thus when and where it can occur on Mars. Our results show that basal
sublimation is possible if we consider large pathlengths and very little
dust content within the ice. Moreover, the model can explain how dark
spots can appear very early after the end of the polar night at high
latitudes. We also evaluate the importance of the different parameters
in our simulations. Contrary to what was suggested by theoretical
models, the role of seasonal thermal waves is found to be limited. Solar
radiation alone can initiate basal sublimation, which therefore only
depends on the CO $_{2}$ ice properties. Three main modes were
identified: one where condensation/sublimation only occurs at the
surface (in the case of small grains and/or high dust content), one
where basal sublimation is possible (large pathlengths and very little
dust content) and an intermediate mode where sublimation within the ice
may occur. We suggest that these different modes could be keys to
understanding many processes that occur at the surface of Mars, like the
anticryptic area behavior or the recent reported activity in gullies.
}},
  doi = {10.1016/j.icarus.2011.01.031},
  adsurl = {http://adsabs.harvard.edu/abs/2011Icar..213..131P},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011Icar..212..504S,
  author = {{Spiga}, A. and {Forget}, F. and {Madeleine}, J.-B. and {Montabone}, L. and 
	{Lewis}, S.~R. and {Millour}, E.},
  title = {{The impact of martian mesoscale winds on surface temperature and on the determination of thermal inertia}},
  journal = {\icarus},
  year = 2011,
  month = apr,
  volume = 212,
  pages = {504-519},
  abstract = {{Radiative control of surface temperature is a key characteristic of the
martian environment and its low-density atmosphere. Here we show through
meteorological modeling that surface temperature can be far from
radiative equilibrium over numerous sloping terrains on Mars, where
nighttime mesoscale katabatic winds impact the surface energy budget.
Katabatic circulations induce both adiabatic atmospheric heating and
enhancement of downward sensible heat flux, which then becomes
comparable to radiative flux and acts to warm the ground. Through this
mechanism, surface temperature can increase up to 20 K. One consequence
is that warm signatures of surface temperature over slopes, observed
through infrared spectrometry, cannot be systematically associated with
contrasts of intrinsic soil thermal inertia. Apparent thermal inertia
maps retrieved thus far possibly contain wind-induced structures.
Another consequence is that surface temperature observations close to
sloping terrains could allow the validation of model predictions for
martian katabatic winds, provided contrasts in intrinsic thermal inertia
can be ruled out. The thermal impact of winds is mostly discussed in
this paper in the particular cases of Olympus Mons/Lycus Sulci and Terra
Meridiani but is generally significant over any sloped terrains in low
thermal inertia areas. It is even general enough to apply under daytime
conditions, thereby providing a possible explanation for observed
afternoon surface cooling, and to ice-covered terrains, thereby
providing new insights on how winds could have shaped the present
surface of Mars.
}},
  doi = {10.1016/j.icarus.2011.02.001},
  adsurl = {http://adsabs.harvard.edu/abs/2011Icar..212..504S},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}