Carbon Dioxide Non-LTE Emission In The Telluric Upper Atmospheres

Details Carbon Dioxide Non-LTE Emission In The Telluric Upper Atmospheres Carbon Dioxide Non-LTE Emission In The Telluric Upper Atmospheres

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.4506d&link_type=abstract

American Astronomical Society, DPS meeting #39, #45.06; Bulletin of the American Astronomical Society, Vol. 39, p.503

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Venus Express observations with VIRTIS (Drossart et al, PSS, 2007), as well as Mars Express with OMEGA (Bibring et al., Nature, 2004) provide regularly limb detection of CO2 non-LTE (fluorescent) emission at 4.3 μm. These emissions come from radiative transition in the low-collisional upper atmospheres of both planets, between 100-120 km on Venus and 80-110 km on Mars. Observations by VIRTIS/Rosetta during the Mars flyby in February 2007 have also provided CO2 fluorescence detection. High resolution (λ/δλ 1500), spatially resolved (3km) spectroscopy of the limb give modelling constraints on the upper atmospheric structure. In addition, nadir observations of the stronger Venus emission with VIRTIS-M mapping channel give access to two dimensional spatial variability studies.
Finally, Earth observations obtained by Rosetta/VIRTIS in March 2005 with Rosetta/VIRTIS, which will be repeated during the November 2007 flyby, have provided limb detection of CO2 emission, very similar to Mars and Venus. A comparison of the three telluric planets CO2 emission with the same instrument on two spacecraft is therefore possible for the first time.

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