Skip to content. | Skip to navigation

Personal tools

You are here: Home / Publications / Peer-reviewed papers / lmd_Hourdin2007_bib.html



@comment{{This file has been generated by bib2bib 1.95}}
@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c 'not journal:"Polymer Science"' -c '  author:"Hourdin"  ' -c year=2007 -c $type="ARTICLE" -oc lmd_Hourdin2007.txt -ob lmd_Hourdin2007.bib /home/WWW/LMD/public/}}
  author = {{Braconnot}, P. and {Hourdin}, F. and {Bony}, S. and {Dufresne}, J.~L. and 
	{Grandpeix}, J.~Y. and {Marti}, O.},
  title = {{Impact of different convective cloud schemes on the simulation of the tropical seasonal cycle in a coupled ocean atmosphere model}},
  journal = {Climate Dynamics},
  keywords = {Orientation-preserving condition, Finite element analysis, Compressible hyperelasticity},
  year = 2007,
  month = oct,
  volume = 29,
  pages = {501},
  abstract = {{The simulation of the mean seasonal cycle of sea surface temperature
(SST) remains a challenge for coupled ocean atmosphere general
circulation models (OAGCMs). Here we investigate how the numerical
representation of clouds and convection affects the simulation of the
seasonal variations of tropical SST. For this purpose, we compare
simulations performed with two versions of the same OAGCM differing only
by their convection and cloud schemes. Most of the atmospheric
temperature and precipitation differences between the two simulations
reflect differences found in atmosphere-alone simulations. They affect
the ocean interior down to 1,000 m. Substantial differences are found
between the two coupled simulations in the seasonal march of the
Intertropical Convergence Zone in the eastern part of the Pacific and
Atlantic basins, where the equatorial upwelling develops. The results
confirm that the distribution of atmospheric convection between ocean
and land during the American and African boreal summer monsoons plays a
key role in maintaining a cross equatorial flow and a strong windstress
along the equator, and thereby the equatorial upwelling. Feedbacks
between convection, large-scale circulation, SST and clouds are
highlighted from the differences between the two simulations. In one
case, these feedbacks maintain the ITCZ in a quite realistic position,
whereas in the other case the ITCZ is located too far south close to the
  doi = {10.1007/s00382-007-0244-y},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Coindreau}, O. and {Hourdin}, F. and {Haeffelin}, M. and {Mathieu}, A. and 
	{Rio}, C.},
  title = {{Assessment of Physical Parameterizations Using a Global Climate Model with Stretchable Grid and Nudging}},
  journal = {Monthly Weather Review},
  year = 2007,
  volume = 135,
  pages = {1474},
  doi = {10.1175/MWR3338.1},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Bertaux}, J.-L. and {Nevejans}, D. and {Korablev}, O. and {Villard}, E. and 
	{Quémerais}, E. and {Neefs}, E. and {Montmessin}, F. and 
	{Leblanc}, F. and {Dubois}, J.~P. and {Dimarellis}, E. and {Hauchecorne}, A. and 
	{Lefèvre}, F. and {Rannou}, P. and {Chaufray}, J.~Y. and 
	{Cabane}, M. and {Cernogora}, G. and {Souchon}, G. and {Semelin}, F. and 
	{Reberac}, A. and {Van Ransbeek}, E. and {Berkenbosch}, S. and 
	{Clairquin}, R. and {Muller}, C. and {Forget}, F. and {Hourdin}, F. and 
	{Talagrand}, O. and {Rodin}, A. and {Fedorova}, A. and {Stepanov}, A. and 
	{Vinogradov}, I. and {Kiselev}, A. and {Kalinnikov}, Y. and 
	{Durry}, G. and {Sandel}, B. and {Stern}, A. and {Gérard}, J.~C.
  title = {{SPICAV on Venus Express: Three spectrometers to study the global structure and composition of the Venus atmosphere}},
  journal = {\planss},
  year = 2007,
  month = oct,
  volume = 55,
  pages = {1673-1700},
  abstract = {{Spectroscopy for the investigation of the characteristics of the
atmosphere of Venus (SPICAV) is a suite of three spectrometers in the UV
and IR range with a total mass of 13.9 kg flying on the Venus Express
(VEX) orbiter, dedicated to the study of the atmosphere of Venus from
ground level to the outermost hydrogen corona at more than 40,000 km. It
is derived from the SPICAM instrument already flying on board Mars
Express (MEX) with great success, with the addition of a new IR
high-resolution spectrometer, solar occultation IR (SOIR), working in
the solar occultation mode. The instrument consists of three
spectrometers and a simple data processing unit providing the interface
of these channels with the spacecraft. A UV spectrometer (118-320 nm,
resolution 1.5 nm) is identical to the MEX version. It is dedicated to
nadir viewing, limb viewing and vertical profiling by stellar and solar
occultation. In nadir orientation, SPICAV UV will analyse the albedo
spectrum (solar light scattered back from the clouds) to retrieve SO
$_{2}$, and the distribution of the UV-blue absorber (of still
unknown origin) on the dayside with implications for cloud structure and
atmospheric dynamics. On the nightside, {$\gamma$} and {$\delta$} bands of NO
will be studied, as well as emissions produced by electron
precipitations. In the stellar occultation mode the UV sensor will
measure the vertical profiles of CO $_{2}$, temperature, SO
$_{2}$, SO, clouds and aerosols. The density/temperature profiles
obtained with SPICAV will constrain and aid in the development of
dynamical atmospheric models, from cloud top ({\tilde}60 km) to 160 km in
the atmosphere. This is essential for future missions that would rely on
aerocapture and aerobraking. UV observations of the upper atmosphere
will allow studies of the ionosphere through the emissions of CO, CO
$^{+}$, and CO $_{2}$$^{+}$, and its direct
interaction with the solar wind. It will study the H corona, with its
two different scale heights, and it will allow a better understanding of
escape mechanisms and estimates of their magnitude, crucial for insight
into the long-term evolution of the atmosphere. The SPICAV VIS-IR sensor
(0.7-1.7 {$\mu$}m, resolution 0.5-1.2 nm) employs a pioneering technology:
an acousto-optical tunable filter (AOTF). On the nightside, it will
study the thermal emission peeping through the clouds, complementing the
observations of both VIRTIS and Planetary Fourier Spectrometer (PFS) on
VEX. In solar occultation mode this channel will study the vertical
structure of H $_{2}$O, CO $_{2}$, and aerosols. The SOIR
spectrometer is a new solar occultation IR spectrometer in the range
{$\lambda$}=2.2-4.3 {$\mu$}m, with a spectral resolution {$\lambda$}/{$\Delta$}
{$\lambda$}{\gt}15,000, the highest on board VEX. This new concept includes
a combination of an echelle grating and an AOTF crystal to sort out one
order at a time. The main objective is to measure HDO and H
$_{2}$O in solar occultation, in order to characterize the escape
of D atoms from the upper atmosphere and give more insight about the
evolution of water on Venus. It will also study isotopes of CO
$_{2}$ and minor species, and provides a sensitive search for new
species in the upper atmosphere of Venus. It will attempt to measure
also the nightside emission, which would allow a sensitive measurement
of HDO in the lower atmosphere, to be compared to the ratio in the upper
atmosphere, and possibly discover new minor atmospheric constituents.
  doi = {10.1016/j.pss.2007.01.016},
  adsurl = {},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
Contact information

EMC3 group

Case 99
Tour 45-55, 3ème étage
4 Place Jussieu
75252 Paris Cedex 05
Tel: 33 + 1 44 27 27 99
      33 + 6 16 27 34 18 (Dr F. Cheruy)
Tel: 33 + 1 44 27 35 25 (Secretary)
Fax: 33 + 1 44 27 62 72
email: emc3 at

Map of our location

Real time LMDZ simulations

Today's LMDZ meteogram for the SIRTA site

Intranet EMC3

Intranet EMC3