@comment{{This file has been generated by bib2bib 1.97}}
@comment{{Command line: bib2bib --quiet -c year=2010 -c $type="ARTICLE" -oc pub2010.txt -ob pub2010.bib}}
  author = {{Cordier}, D. and {Mousis}, O. and {Lunine}, J.~I. and {Lebonnois}, S. and 
	{Lavvas}, P. and {Lobo}, L.~Q. and {Ferreira}, A.~G.~M.},
  title = {{About the Possible Role of Hydrocarbon Lakes in the Origin of Titan's Noble Gas Atmospheric Depletion}},
  journal = {\apjl},
  archiveprefix = {arXiv},
  eprint = {1008.3712},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: atmospheres, planets and satellites: individual: Titan, planets and satellites: general},
  year = 2010,
  volume = 721,
  pages = {L117-L120},
  abstract = {{An unexpected feature of Titan's atmosphere is the strong depletion in
primordial noble gases revealed by the Gas Chromatograph Mass
Spectrometer aboard the Huygens probe during its descent on 2005 January
14. Although several plausible explanations have already been
formulated, no definitive response to this issue has yet been found.
Here, we investigate the possible sequestration of these noble gases in
the liquid contained in lakes and wet terrains on Titan and the
consequences for their atmospheric abundances. Considering the
atmosphere and the liquid existing on the soil as a whole system, we
compute the abundance of each noble gas relative to nitrogen. To do so,
we make the assumption of thermodynamic equilibrium between the liquid
and the atmosphere, the abundances of the different constituents being
determined via regular solution theory. We find that xenon's atmospheric
depletion can be explained by its dissolution at ambient temperature in
the liquid presumably present on Titan's soil. In the cases of argon and
krypton, we find that the fractions incorporated in the liquid are
negligible, implying that an alternative mechanism must be invoked to
explain their atmospheric depletion.
  doi = {10.1088/2041-8205/721/2/L117},
  adsurl = {},
  localpdf = {REF/2010ApJ...721L.117C.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Grassi}, D. and {Migliorini}, A. and {Montabone}, L. and {Lebonnois}, S. and 
	{Cardes{\`i}n-Moinelo}, A. and {Piccioni}, G. and {Drossart}, P. and 
	{Zasova}, L.~V.},
  title = {{Thermal structure of Venusian nighttime mesosphere as observed by VIRTIS-Venus Express}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Atmospheric Composition and Structure: Planetary atmospheres (5210, 5405, 5704), Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Remote sensing, Planetary Sciences: Solar System Objects: Venus},
  year = 2010,
  volume = 115,
  eid = {E09007},
  pages = {9007},
  abstract = {{The mapping IR channel of the Visual and Infrared Thermal Imaging
Spectrometer (VIRTIS-M) on board the Venus Express spacecraft observes
the CO$_{2}$ band at 4.3 {$\mu$}m at a spectral resolution adequate
to retrieve the atmospheric temperature profiles in the 65-96 km
altitude range. Observations acquired in the period June 2006 to July
2008 were used to derive average temperature fields as a function of
latitude, subsolar longitude (i.e., local time, LT), and pressure.
Coverage presented here is limited to the nighttime because of the
adverse effects of daytime non-LTE emission on the retrieval procedure
and to southernmost latitudes because of the orientation of the
Venus-Express orbit. Maps of air temperature variability are also
presented as the standard deviation of the population included in each
averaging bin. At the 100 mbar level (about 65 km above the reference
surface), temperatures tend to decrease from the evening to the morning
side despite a local maximum observed around 20-21LT. The cold collar is
evident around 65S, with a minimum temperature at 3LT. Moving to higher
altitudes, local time trends become less evident at 12.6 mbar (about 75
km) where the temperature monotonically increases from middle latitudes
to the southern pole. Nonetheless, at this pressure level, two weaker
local time temperature minima are observed at 23LT and 2LT equatorward
of 60S. Local time trends in temperature reverse about 85 km, where the
morning side is the warmer. The variability at the 100 mbar level is
maximum around 80S and stronger toward the morning side. Moving to
higher altitudes, the morning side always shows the stronger
variability. Southward of 60S, standard deviation presents minimum
values around 12.6 mbar for all the local times.
  doi = {10.1029/2009JE003553},
  adsurl = {},
  localpdf = {REF/2010JGRE..115.9007G.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Lebonnois}, S. and {Hourdin}, F. and {Eymet}, V. and {Crespin}, A. and 
	{Fournier}, R. and {Forget}, F.},
  title = {{Superrotation of Venus' atmosphere analyzed with a full general circulation model}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Planetary Sciences: Solid Surface Planets: Meteorology (3346), Atmospheric Processes: Planetary meteorology (5445, 5739), Atmospheric Composition and Structure: Planetary atmospheres (5210, 5405, 5704), Atmospheric Processes: General circulation (1223)},
  year = 2010,
  volume = 115,
  eid = {E06006},
  pages = {6006},
  abstract = {{A general circulation model (GCM) has been developed for the Venus
atmosphere, from the surface up to 100 km altitude, based on the GCM
developed for Earth at our laboratory. Key features of this new GCM
include topography, diurnal cycle, dependence of the specific heat on
temperature, and a consistent radiative transfer module based on net
exchange rate matrices. This allows a consistent computation of the
temperature field, in contrast to previous GCMs of Venus atmosphere that
used simplified temperature forcing. The circulation is analyzed after
350 Venus days (111 Earth years). Superrotation is obtained above
roughly 40 km altitude. Below, the zonal wind remains very small
compared to observed values, which is a major pending question. The
meridional circulation consists of equator-to-pole cells, the dominant
one being located within the cloud layers. The modeled temperature
structure is globally consistent with observations, though discrepancies
persist in the stability of the lowest layers and equator-pole
temperature contrast within the clouds (10 K in the model compared to
the observed 40 K). In agreement with observational data, a convective
layer is found between the base of the clouds (around 47 km) and the
middle of the clouds (55-60 km altitude). The transport of angular
momentum is analyzed, and comparison between the reference simulation
and a simulation without diurnal cycle illustrates the role played by
thermal tides in the equatorial region. Without diurnal cycle, the
Gierasch-Rossow-Williams mechanism controls angular momentum transport.
The diurnal tides add a significant downward transport of momentum in
the equatorial region, causing low latitude momentum accumulation.
  doi = {10.1029/2009JE003458},
  adsurl = {},
  localpdf = {REF/2010JGRE..115.6006L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}