lmd_Hourdin2002.bib

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@article{2002Natur.418..853R,
  author = {{Rannou}, P. and {Hourdin}, F. and {McKay}, C.~P.},
  title = {{A wind origin for Titan's haze structure}},
  journal = {\nat},
  year = 2002,
  month = aug,
  volume = 418,
  pages = {853-856},
  abstract = {{Titan, the largest moon of Saturn, is the only satellite in the Solar
System with a dense atmosphere. Titan's atmosphere is mainly nitrogen
with a surface pressure of 1.5atmospheres and a temperature of 95K (ref.
1). A seasonally varying haze, which appears to be the main source of
heating and cooling that drives atmospheric circulation, shrouds the
moon. The haze has numerous features that have remained unexplained.
There are several layers, including a `polar hood', and a pronounced
hemispheric asymmetry. The upper atmosphere rotates much faster than the
surface of the moon, and there is a significant latitudinal temperature
asymmetry at the equinoxes. Here we describe a numerical simulation of
Titan's atmosphere, which appears to explain the observed features of
the haze. The critical new factor in our model is the coupling of haze
formation with atmospheric dynamics, which includes a component of
strong positive feedback between the haze and the winds.
}},
  adsurl = {http://adsabs.harvard.edu/abs/2002Natur.418..853R},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2002JGRE..107.5055V,
  author = {{Van den Acker}, E. and {Van Hoolst}, T. and {de Viron}, O. and 
	{Defraigne}, P. and {Forget}, F. and {Hourdin}, F. and {Dehant}, V.
	},
  title = {{Influence of the seasonal winds and the CO$_{2}$ mass exchange between atmosphere and polar caps on Mars' rotation}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Planetary Sciences: Orbital and rotational dynamics, Planetary Sciences: Interiors (8147), Planetary Sciences: Atmospheres-structure and dynamics, Planetary Sciences: Polar regions,},
  year = 2002,
  month = jul,
  volume = 107,
  eid = {5055},
  pages = {5055},
  abstract = {{The Martian atmosphere and the CO$_{2}$ polar ice caps exchange
mass. This exchange, together with the atmospheric response to solar
heating, induces variations of the rotation of Mars. Using the angular
momentum budget equation of the system solid-Mars-atmosphere-polar ice
caps, the variations of Mars' rotation can be deduced from the
variations of the angular momentum of the superficial layer; this later
is associated with the winds, that is, the motion term, and with the
mass redistribution, that is, the matter term. For the ``mean'' Martian
atmosphere, without global dust storms, total amplitudes of 10 cm on the
surface are obtained for both the annual and semiannual polar motion
excited by the atmosphere and ice caps. The atmospheric pressure
variations are the dominant contribution to these amplitudes.
Length-of-day (lod) variations have amplitudes of 0.253 ms for the
annual signal and of 0.246 ms for the semiannual signal. The lod
variations are mainly associated with changes in the atmospheric
contribution to the mass term, partly compensated by the polar ice cap
contribution. We computed lod variations and polar motion for three
scenarios having different atmospheric dust contents. The differences
between the three sets of results for lod variations are about one order
of magnitude larger than the expected accuracy of the NEtlander
Ionosphere and Geodesy Experiment (NEIGE) for lod. It will thus be
possible to constrain the global atmospheric circulation models from the
NEIGE measurements.
}},
  doi = {10.1029/2000JE001539},
  adsurl = {http://adsabs.harvard.edu/abs/2002JGRE..107.5055V},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2002JAtS...59.1105H,
  author = {{Hourdin}, F. and {Couvreux}, F. and {Menut}, L.},
  title = {{Parameterization of the Dry Convective Boundary Layer Based on a Mass Flux Representation of Thermals.}},
  journal = {Journal of Atmospheric Sciences},
  year = 2002,
  month = mar,
  volume = 59,
  pages = {1105-1123},
  abstract = {{Presented is a mass flux parameterization of vertical transport in the
convective boundary layer. The formulation of the new parameterization
is based on an idealization of thermal cells or rolls. The
parameterization is validated by comparison to large eddy simulations
(LES). It is also compared to classical boundary layer schemes on a
documented case of a well-developed convective boundary layer observed
in the Paris area during the {\'E}tude et Simulation de la
Qualité de l'air en Ile de France (ESQUIF) campaign. For both LES
and observations, the new scheme performs better at simulating
entrainment fluxes at the top of the convective boundary layer and at
near-surface conditions. The explicit representation of mass fluxes
allows a direct comparison with campaign observations and opens
interesting possibilities for coupling with clouds and deep convection
schemes.
}},
  doi = {10.1175/1520-0469(2002)059<1105:POTDCB>2.0.CO;2},
  adsurl = {http://adsabs.harvard.edu/abs/2002JAtS...59.1105H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}