lmd_Madeleine2010.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=2010 -c $type="ARTICLE" -oc lmd_Madeleine2010.txt -ob lmd_Madeleine2010.bib /home/WWW/LMD/public/Publis_LMDEMC3.link.bib}}
@article{2010A&A...522A..22W;,
author = {{Wordsworth}, R.~D. and {Forget}, F. and {Selsis}, F. and {Madeleine}, J.-B. and
{Millour}, E. and {Eymet}, V.},
title = {{Is Gliese 581d habitable? Some constraints from radiative-convective climate modeling}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1005.5098},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: atmospheres, planets and satellites: surfaces, planetary systems, planet-star interactions, convection, radiative transfer},
year = 2010,
month = nov,
volume = 522,
eid = {A22},
pages = {A22},
abstract = {{The recently discovered exoplanet Gl 581d is extremely close to the
outer edge of its system's habitable zone, which has led to much
speculation on its possible climate. We have performed a range of
simulations to assess whether, given simple combinations of chemically
stable greenhouse gases, the planet could sustain liquid water on its
surface. For best estimates of the surface gravity, surface albedo and
cloud coverage, we find that less than 10 bars of CO$_{2}$ is
sufficient to maintain a global mean temperature above the melting point
of water. Furthermore, even with the most conservative choices of these
parameters, we calculate temperatures above the water melting point for
CO$_{2}$ partial pressures greater than about 40 bar. However, we
note that as Gl 581d is probably in a tidally resonant orbit, further
simulations in 3D are required to test whether such atmospheric
conditions are stable against the collapse of CO$_{2}$ on the
surface.
}},
doi = {10.1051/0004-6361/201015053},
adsurl = {http://adsabs.harvard.edu/abs/2010A%26A...522A..22W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2010Icar..208..658M,
author = {{Morgan}, G.~A. and {Head}, J.~W. and {Forget}, F. and {Madeleine}, J.-B. and
{Spiga}, A.},
title = {{Gully formation on Mars: Two recent phases of formation suggested by links between morphology, slope orientation and insolation history}},
journal = {\icarus},
year = 2010,
month = aug,
volume = 208,
pages = {658-666},
abstract = {{The unusual 80 km diameter Noachian-aged Asimov crater in Noachis Terra
(46{\deg}S, 5{\deg}E) is characterized by extensive Noachian-Hesperian
crater fill and a younger superposed annulus of valleys encircling the
margins of the crater floor. These valleys provide an opportunity to
study the relationships of gully geomorphology as a function of changing
slope orientation relative to solar insolation. We found that the level
of development of gullies was highly correlated with slope orientation
and solar insolation. The largest and most complex gully systems, with
the most well-developed fluvial landforms, are restricted to pole-facing
slopes. In contrast, gullies on equator-facing slopes are smaller, more
poorly developed and integrated, more highly degraded, and contain more
impact craters. We used a 1D version of the Laboratoire de
Météorologie Dynamique GCM, and slope geometries
(orientation and angle), driven by predicted spin-axis/orbital parameter
history, to assess the distribution and history of surface temperatures
in these valleys during recent geological history. Surface temperatures
on pole-facing slopes preferential for water ice accumulation and
subsequent melting are predicted to occur as recently as 0.5-2.1 Ma,
which is consistent with age estimates of gully activity elsewhere on
Mars. In contrast, the 1D model predicts that water ice cannot
accumulate on equator-facing slopes until obliquities exceed 45{\deg},
suggesting they are unlikely to have been active over the last 5 Ma. The
correlation of the temperature predictions and the geological evidence
for age differences suggests that there were two phases of gully
formation in the last few million years: an older phase in which
top-down melting occurred on equator-facing slopes and a younger more
robust phase on pole-facing slopes. The similarities of small-scale
fluvial erosion features seen in the gullies on Mars and those observed
in gullies cut by seasonal and perennial snowmelt in the Antarctic Dry
Valleys supports a top-down melting origin for these gullies on Mars.
}},
doi = {10.1016/j.icarus.2010.02.019},
adsurl = {http://adsabs.harvard.edu/abs/2010Icar..208..658M},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
