lmd_Madeleine2014.bib
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@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c 'not journal:"Polymer Science"' -c ' author:"Madeleine" ' -c year=2014 -c $type="ARTICLE" -oc lmd_Madeleine2014.txt -ob lmd_Madeleine2014.bib /home/WWW/LMD/public/Publis_LMDEMC3.link.bib}}
@article{2014JGRE..119.1479N,
author = {{Navarro}, T. and {Madeleine}, J.-B. and {Forget}, F. and {Spiga}, A. and
{Millour}, E. and {Montmessin}, F. and {M{\"a}{\"a}tt{\"a}nen}, A.
},
title = {{Global climate modeling of the Martian water cycle with improved microphysics and radiatively active water ice clouds}},
journal = {Journal of Geophysical Research (Planets)},
archiveprefix = {arXiv},
eprint = {1310.1010},
primaryclass = {astro-ph.EP},
keywords = {Mars, atmosphere, climate, global climate model, clouds, water},
year = 2014,
month = jul,
volume = 119,
pages = {1479-1495},
abstract = {{Water ice clouds play a key role in the radiative transfer of the
Martian atmosphere, impacting its thermal structure, its circulation,
and, in turn, the water cycle. Recent studies including the radiative
effects of clouds in global climate models (GCMs) have found that the
corresponding feedbacks amplify the model defaults. In particular, it
prevents models with simple microphysics from reproducing even the basic
characteristics of the water cycle. Within that context, we propose a
new implementation of the water cycle in GCMs, including a detailed
cloud microphysics taking into account nucleation on dust particles, ice
particle growth, and scavenging of dust particles due to the
condensation of ice. We implement these new methods in the Laboratoire
de Météorologie Dynamique GCM and find satisfying
agreement with the Thermal Emission Spectrometer observations of both
water vapor and cloud opacities, with a significant improvement when
compared to GCMs taking into account radiative effects of water ice
clouds without this implementation. However, a lack of water vapor in
the tropics after Ls = 180{\deg} is persistent in simulations compared to
observations, as a consequence of aphelion cloud radiative effects
strengthening the Hadley cell. Our improvements also allow us to explore
questions raised by recent observations of the Martian atmosphere.
Supersaturation above the hygropause is predicted in line with
Spectroscopy for Investigation of Characteristics of the Atmosphere of
Mars observations. The model also suggests for the first time that the
scavenging of dust by water ice clouds alone fails to fully account for
the detached dust layers observed by the Mars Climate Sounder.
}},
doi = {10.1002/2013JE004550},
adsurl = {http://adsabs.harvard.edu/abs/2014JGRE..119.1479N},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2014GeoRL..41.4873M,
author = {{Madeleine}, J.-B. and {Head}, J.~W. and {Forget}, F. and {Navarro}, T. and
{Millour}, E. and {Spiga}, A. and {Cola{\"i}tis}, A. and {M{\"a}{\"a}tt{\"a}nen}, A. and
{Montmessin}, F. and {Dickson}, J.~L.},
title = {{Recent Ice Ages on Mars: The role of radiatively active clouds and cloud microphysics}},
journal = {\grl},
keywords = {Glaciation, Mars, Paleoclimate, Climate model, Clouds, Climate},
year = 2014,
month = jul,
volume = 41,
pages = {4873-4879},
abstract = {{Global climate models (GCMs) have been successfully employed to explain
the origin of many glacial deposits on Mars. However, the
latitude-dependent mantle (LDM), a dust-ice mantling deposit that is
thought to represent a recent ''Ice Age,'' remains poorly explained by
GCMs. We reexamine this question by considering the effect of
radiatively active water-ice clouds (RACs) and cloud microphysics. We
find that when obliquity is set to 35{\deg}, as often occurred in the
past 2 million years, warming of the atmosphere and polar caps by clouds
modifies the water cycle and leads to the formation of a several
centimeter-thick ice mantle poleward of 30{\deg} in each hemisphere
during winter. This mantle can be preserved over the summer if increased
atmospheric dust content obscures the surface and provides dust nuclei
to low-altitude clouds. We outline a scenario for its deposition and
preservation that compares favorably with the characteristics of the
LDM.
}},
doi = {10.1002/2014GL059861},
adsurl = {http://adsabs.harvard.edu/abs/2014GeoRL..41.4873M},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
