pub2013.bib

@comment{{This file has been generated by bib2bib 1.97}}

@comment{{Command line: bib2bib --quiet -c year=2013 -c $type="ARTICLE" -oc pub2013.txt -ob pub2013.bib lebonnois.link.bib}}

@article{2013JGRE..118.1983M,
  author = {{Marcq}, E. and {Lebonnois}, S.},
  title = {{Simulations of the latitudinal variability of CO-like and OCS-like passive tracers below the clouds of Venus using the Laboratoire de Météorologie Dynamique GCM}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Venus, atmosphere, general circulation model, passive tracers, carbon monoxide, carbonyl sulfide},
  year = 2013,
  volume = 118,
  pages = {1983-1990},
  abstract = {{The lower atmosphere of Venus below the clouds is a transitional region
between the relatively calm lowermost scale height and the superrotating
atmosphere in the cloud region and above. Any observational constraint
is then welcome to help in the development of general circulation models
of Venus, a difficult task considering the thickness of its atmosphere.
Starting from a state-of-the-art 3-D Venus General Circulation Model
(GCM), we have included passive tracers in order to investigate the
latitudinal variability of two minor gaseous species, carbonyl sulfide
(OCS) and carbon monoxide (CO), whose vertical profiles and mixing
ratios are known to vary with latitude between 30 and 40km. The
relaxation to chemical equilibrium is crudely parametrized through a
vertically uniform time scale {$\tau$}. A satisfactory agreement with
available observations is obtained with
10$^{8}$s{\lsim}{$\tau$}$_{CO}${\lsim}5{\middot}10$^{8}$ s
and 10$^{7}$s{\lsim}{$\tau$}$_{OCS}${\lsim}10$^{8}$ s.
These results, in addition to validating the general circulation below
the clouds, are also helpful in characterizing the chemical kinetics of
Venus' atmosphere. This complements the much more sophisticated chemical
models which focus more on thermodynamical equilibrium.
}},
  doi = {10.1002/jgre.20146},
  adsurl = {http://cdsads.u-strasbg.fr/abs/2013JGRE..118.1983M},
  localpdf = {REF/2013JGRE..118.1983M.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2013Icar..223..330G,
  author = {{Gans}, B. and {Peng}, Z. and {Carrasco}, N. and {Gauyacq}, D. and 
	{Lebonnois}, S. and {Pernot}, P.},
  title = {{Impact of a new wavelength-dependent representation of methane photolysis branching ratios on the modeling of Titan's atmospheric photochemistry}},
  journal = {\icarus},
  year = 2013,
  volume = 223,
  pages = {330-343},
  abstract = {{A new wavelength-dependent model for CH$_{4}$ photolysis branching
ratios is proposed, based on the values measured recently by Gans et al.
(Gans, B. et al. [2011]. Phys. Chem. Chem. Phys. 13, 8140-8152). We
quantify the impact of this representation on the predictions of a
photochemical model of Titan's atmosphere, on their precision, and
compare to earlier representations. Although the observed effects on the
mole fraction of the species are small (never larger than 50\%), it is
possible to draw some recommendations for further studies: (i) the
Ly-{$\alpha$} branching ratios of Wang et al. (Wang, J.H. et al. [2000]. J.
Chem. Phys. 113, 4146-4152) used in recent models overestimate the
CH$_{2}$:CH$_{3}$ ratio, a factor to which a lot of species
are sensitive; (ii) the description of out-of-Ly-{$\alpha$} branching
ratios by the ''100\% CH$_{3}$'' scenario has to be avoided, as it
can bias significantly the mole fractions of some important species
(C$_{3}$H$_{8}$); and (iii) complementary experimental data
in the 130-140 nm range would be useful to constrain the models in the
Ly-{$\alpha$} deprived 500-700 km altitude range.
}},
  doi = {10.1016/j.icarus.2012.11.024},
  adsurl = {http://cdsads.u-strasbg.fr/abs/2013Icar..223..330G},
  localpdf = {REF/2013Icar..223..330G.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}