@comment{{This file has been generated by bib2bib 1.97}}
@comment{{Command line: bib2bib --quiet -c year=2005 -c $type="ARTICLE" -oc pub2005.txt -ob pub2005.bib}}
  author = {{Encrenaz}, T. and {Bézard}, B. and {Owen}, T. and {Lebonnois}, S. and 
	{Lefèvre}, F. and {Greathouse}, T. and {Richter}, M. and 
	{Lacy}, J. and {Atreya}, S. and {Wong}, A.~S. and {Forget}, F.
  title = {{Infrared imaging spectroscopy of Mars: H $_{2}$O mapping and determination of CO $_{2}$ isotopic ratios}},
  journal = {\icarus},
  year = 2005,
  volume = 179,
  pages = {43-54},
  abstract = {{High-resolution infrared imaging spectroscopy of Mars has been achieved
at the NASA Infrared Telescope Facility (IRTF) on June 19-21, 2003,
using the Texas Echelon Cross Echelle Spectrograph (TEXES). The
areocentric longitude was 206{\deg}. Following the detection and mapping
of hydrogen peroxide H $_{2}$O $_{2}$ [Encrenaz et al.,
2004. Icarus 170, 424-429], we have derived, using the same data set, a
map of the water vapor abundance. The results appear in good overall
agreement with the TES results and with the predictions of the Global
Circulation Model (GCM) developed at the Laboratory of Dynamical
Meteorology (LMD), with a maximum abundance of water vapor of
3{\plusmn}1.5{\times}10(17{\plusmn}9 pr-{$\mu$}m). We have searched for CH
$_{4}$ over the martian disk, but were unable to detect it. Our
upper limits are consistent with earlier reports on the methane
abundance on Mars. Finally, we have obtained new measurements of CO
$_{2}$ isotopic ratios in Mars. As compared to the terrestrial
values, these values are: ( $^{18}$O/ $^{17}$O)[M/E] = 1.03
{\plusmn} 0.09; ( $^{13}$C/ $^{12}$C)[M/E] = 1.00 {\plusmn}
0.11. In conclusion, in contrast with the analysis of Krasnopolsky et
al. [1996. Icarus 124, 553-568], we conclude that the derived martian
isotopic ratios do not show evidence for a departure from their
terrestrial values.
  doi = {10.1016/j.icarus.2005.06.022},
  adsurl = {},
  localpdf = {REF/2005Icar..179...43E.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Lebonnois}, S.},
  title = {{Benzene and aerosol production in Titan and Jupiter's atmospheres: a sensitivity study}},
  journal = {\planss},
  year = 2005,
  volume = 53,
  pages = {486-497},
  abstract = {{Benzene has recently been observed in the atmosphere of Jupiter, Saturn
and also Titan. This compound is required as a precursor for larger
aromatic species (PAHs) that may be part of aerosol particles. Several
photochemical models have tried to reproduce the observed quantities of
benzene in the atmospheres of Jupiter (both low- and high-latitudes
regions), Saturn and Titan. In this present work, we have conducted a
sensitivity study of benzene and PAHs formation, using similar
photochemical schemes both for Titan and Jupiter (low-latitudes
conditions). Two different photochemical schemes are used, for which the
modeled composition fairly agrees with observational constraints, both
for Jupiter and Titan. Some disagreements are specific to each
atmospheric case, which may point to needed improvements, especially in
kinetic data involved in the corresponding chemical cycles. The observed
benzene mole fraction in Titan's stratosphere is reproduced by the
model, but in the case of Jupiter, low-latitudes benzene abundance is
only 3\% of the observed column density, which may indicate a possible
influence of latitudinal transport, since abundance of benzene is much
higher in auroral regions. Though, the photochemical scheme of
C$_{6}$ compounds at temperature and pressure conditions of
planetary atmospheres is still very uncertain. Several variations are
therefore done on key reactions in benzene production. These variations
show that benzene abundance is mainly sensitive to reactions that may
affect the propargyl radical. The effect of aerosol production on
hydrocarbons composition is also tested, as well as possible
heterogenous recombination of atomic hydrogen in the case of Titan. PAHs
are a major pathway for aerosol production in both models. The mass
production profiles for aerosols are discussed for both Titan and
Jupiter. Total production mass fluxes are roughly three times the one
expected by observational constraints in both cases. Such comparative
studies are useful to bring more constraints on photochemical models.
  doi = {10.1016/j.pss.2004.11.004},
  adsurl = {},
  localpdf = {REF/2005P_26SS...53..486L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Rannou}, P. and {Lebonnois}, S. and {Hourdin}, F. and {Luz}, D.
  title = {{Titan atmosphere database}},
  journal = {Advances in Space Research},
  year = 2005,
  volume = 36,
  pages = {2194-2198},
  abstract = {{We have developed in the last decade a two-dimensional version of the
Titan global circulation model LMDZ. This model accounts for multiple
coupling occuring on Titan between dynamics, haze, chemistry and
radiative transfer. It was successful at explaining many observed
features related to atmosphere state (wind, temperature), haze structure
and chemical species distributions, recently, an important step in our
knowledge about Titan has been done with Cassini and Huygens visits to
Titan. In this context, we want to make the results of our model
available for the scientific community which is involved in the study of
Titan. Such a tool should be useful to give a global frame (spatial and
time behaviour of physical quantities) for interpreting ground based
telescope observations.
  doi = {10.1016/j.asr.2005.09.041},
  adsurl = {},
  localpdf = {REF/2005AdSpR..36.2194R.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}