Observations millimétriques et submillimétriques des composés oxygénés dans les atmosphères planétaires. Préparation aux missions Herschel et ALMA

Details Observations millimétriques et submillimétriques des composés oxygénés dans les atmosphères planétaires. Préparation aux missions Herschel et ALMA Observations millimétriques et submillimétriques des composés oxygénés dans les atmosphères planétaires. Préparation aux missions Herschel et ALMA

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008phdt........22c&link_type=abstract

PhD Thesis, Université Bordeaux 1, cavalie@obs.u-bordeaux1.fr

Computer Science

Solar System, Giant Planets, Mars, Atmosphere, (Sub)Millimeter Spectroscopy, Radiative Transfer, Photochemistry, Oxygen Compounds, Herschel, Alma

Scientific paper

The planetary atmospheres can be characterized by observations carried out in the millimeter and submillimeter wavelength ranges. In a near future, the Herschel Space Observatory as well as the ALMA interferometer will increase our knowledge of the planet atmospheres.
One of the main goals of this thesis work consists in developing an analysis tool for millimeter and submillimeter observations, which will be carried out with Herschel and ALMA. The model we have developed takes into account the spherical geometry of the planets and the properties of the telescopes.
First, we have studied the origin of oxygen compounds in the atmospheres of the giant planets. We have validated our radiative transfer model from this study. We present the analysis of observations of carbon monoxide in the atmospheres of Saturn and Uranus, which have been carried out with the IRAM and JCMT telescopes, in order to constrain the origin of this compound. We improve existing upper limits and prove the existence of an external source of carbon monoxide in the atmosphere of Saturn from the first observation of this compound at submillimeter wavelengths. We also analyse recent observations from the Odin space telescope of water vapor in the stratosphere of Jupiter to constrain its external source. We confirm that the observed water is probably mostly due to the collision of comet Shoemaker-Levy 9 with the planet.
Then, we have used our model in order to study the thermal structure as well as the dynamics of the atmosphere of Mars from carbon monoxide observations. These observations are compared to predictions of a general circulation model to check the consistency of the predictions. They also provide new observational constraints to general circulation models.
Finally, we have used our model to study the atmospheres of the giant planets in the frame of the Herschel guaranteed time key-program "Water and related chemistry in the Solar System". We have also determined the upgrades to implement in our model to analyse ALMA observational data.

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