lmd_Hourdin2000.bib
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@article{2000P&SS...48.1303B;,
author = {{Bertaux}, J.-L. and {Fonteyn}, D. and {Korablev}, O. and {Chassefière}, E. and
{Dimarellis}, E. and {Dubois}, J.~P. and {Hauchecorne}, A. and
{Cabane}, M. and {Rannou}, P. and {Levasseur-Regourd}, A.~C. and
{Cernogora}, G. and {Quemerais}, E. and {Hermans}, C. and {Kockarts}, G. and
{Lippens}, C. and {Maziere}, M.~D. and {Moreau}, D. and {Muller}, C. and
{Neefs}, B. and {Simon}, P.~C. and {Forget}, F. and {Hourdin}, F. and
{Talagrand}, O. and {Moroz}, V.~I. and {Rodin}, A. and {Sandel}, B. and
{Stern}, A.},
title = {{The study of the martian atmosphere from top to bottom with SPICAM light on mars express}},
journal = {\planss},
year = 2000,
month = oct,
volume = 48,
pages = {1303-1320},
abstract = {{SPICAM Light is a small UV-IR instrument selected for Mars Express to
recover most of the science that was lost with the demise of Mars 96,
where the SPICAM set of sensors was dedicated to the study of the
atmosphere of Mars (Spectroscopy for the investigation of the
characteristics of the atmosphere of mars). The new configuration of
SPICAM Light includes optical sensors and an electronics block. A UV
spectrometer (118-320 nm, resolution 0.8 nm) is dedicated to Nadir
viewing, limb viewing and vertical profiling by stellar occultation (3.8
kg). It addresses key issues about ozone, its coupling with H
$_{2}$O, aerosols, atmospheric vertical temperature structure and
ionospheric studies. An IR spectrometer (1.2- 4.8 {$\mu$}m, resolution
0.4-1 nm) is dedicated to vertical profiling during solar occultation of
H $_{2}$O, CO $_{2}$, CO, aerosols and exploration of carbon
compounds (3.5 kg). A nadir looking sensor for H $_{2}$O
abundances (1.0- 1.7 {$\mu$}m, resolution 0.8 nm) is recently included in
the package (0.8 kg). A simple data processing unit (DPU, 0.9 kg)
provides the interface of these sensors with the spacecraft. In nadir
orientation, SPICAM UV is essentially an ozone detector, measuring the
strongest O $_{3}$ absorption band at 250 nm in the spectrum of
the solar light scattered back from the ground. In the stellar
occultation mode the UV Sensor will measure the vertical profiles of CO
$_{2}$, temperature, O $_{3}$, clouds and aerosols. The
density/temperature profiles obtained with SPICAM Light will constrain
and aid in the development of the meteorological and dynamical
atmospheric models, from the surface to 160 km in the atmosphere. This
is essential for future missions that will rely on aerocapture and
aerobraking. UV observations of the upper atmosphere will allow study of
the ionosphere through the emissions of CO, CO $^{+}$, and CO
$_{2}$$^{+}$, and its direct interaction with the solar
wind. Also, 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 SPICAM Light IR sensor is inherited
from the IR solar part of the SPICAM solar occultation instrument of
Mars 96. Its main scientific objective is the global mapping of the
vertical structure of H $_{2}$O, CO $_{2}$, CO, HDO,
aerosols, atmospheric density, and temperature by the solar occultation.
The wide spectral range of the IR spectrometer and its high spectral
resolution allow an exploratory investigation addressing fundamental
question of the possible presence of carbon compounds in the Martian
atmosphere. Because of severe mass constraints this channel is still
optional. An additional nadir near IR channel that employs a pioneering
technology acousto-optical tuneable filter (AOTF) is dedicated to the
measurement of water vapour column abundance in the IR simultaneously
with ozone measured in the UV. It will be done at much lower telemetry
budget compared to the other instrument of the mission, planetary
fourier spectrometer (PFS).
}},
doi = {10.1016/S0032-0633(00)00111-2},
adsurl = {http://adsabs.harvard.edu/abs/2000P%26SS...48.1303B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2000JGR...10524563D,
author = {{Defraigne}, P. and {de Viron}, O. and {Dehant}, V. and {Van Hoolst}, T. and
{Hourdin}, F.},
title = {{Mars rotation variations induced by atmosphere and ice caps}},
journal = {\jgr},
keywords = {Planetology: Solid Surface Planets: Interiors, Planetology: Solid Surface Planets: Orbital and rotational dynamics, Planetology: Solar System Objects: Mars},
year = 2000,
month = oct,
volume = 105,
pages = {24563-24570},
abstract = {{Because of the conservation of angular momentum, the atmospheric winds
and the mass exchange between the Martian ice caps and atmosphere,
associated with the sublimation/condensation process (mainly
CO$_{2}$), induce seasonal effects on Mars' polar motion,
nutation, and length of day (LOD). These effects are computed using the
output of a global circulation model of the Martian atmosphere,
providing atmospheric pressure fields, ice cap surface pressure fields,
and zonal as well as meridional winds. For the LOD variations, total
amplitudes (CO$_{2}$ and wind effects) of 0.22 ms for the annual
wave and of 0.38 ms for the semiannual wave are obtained. These
amplitudes are more than one order of magnitude larger than the LOD
variations induced by the zonal tides, which are at the level of 10
{$\mu$}s. For the induced polar motion the annual amplitude is \~{}11
milliarcseconds (mas), and the semiannual amplitude is \~{}3 mas. The
effect on the nutations, related to the diurnal forcing, is at the level
of 0.1 mas. The differences between the results for a liquid and for a
solid core are examined and shown to be {\lt}1\% of the total effects.
}},
doi = {10.1029/1999JE001227},
adsurl = {http://adsabs.harvard.edu/abs/2000JGR...10524563D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2000GeoRL..27.2245H,
author = {{Hourdin}, F. and {Issartel}, J.-P.},
title = {{Sub-surface nuclear tests monitoring through the CTBT Xenon Network}},
journal = {\grl},
keywords = {Atmospheric Composition and Structure, Atmospheric Composition and Structure: Pollution-urban and regional (0305), Mathematical Geophysics: Inverse theory},
year = 2000,
month = aug,
volume = 27,
pages = {2245-2248},
abstract = {{ We present the first evaluation of the atmospheric xenon network to be
installed as part of the International Monitoring System (IMS) in the
frame of the Comprehensive Test Ban Treaty (CTBT). We show that this
network should, by itself, provide a significant contribution to the
total efficiency of the IMS. For this evaluation, we introduce an
inverse approach based upon the time symmetry of the atmospheric
transport of trace species. This approach may find applications in a
variety of environmental problems.
}},
doi = {10.1029/1999GL010909},
adsurl = {http://adsabs.harvard.edu/abs/2000GeoRL..27.2245H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
