Coradini, A. and Grassi, D. and Capaccioni, F. and Filacchione, G. and Tosi, F. and Ammannito, E. and De Sanctis, M. C. and Formisano, V. and Wolkenberg, P. and Rinaldi, G. and Arnold, G. and Barucci, M. A. and Bellucci, G. and Benkhoff, J. and Bibring, J. P. and Blanco, A. and Bockelee-Morvan, D. and Capria, M. T. and Carlson, R. and Carsenty, U. and Cerroni, P. and Colangeli, L. and Combes, M. and Combi, M. and Crovisier, J. and Drossart, P. and Encrenaz, T. and Erard, S. and Federico, C. and Fink, U. and Fonti, S. and Ip, W.-H. and Irwin, P. G. J. and Jaumann, R. and Kührt, E. and Langevin, Y. and Magni, G. and McCord, T. and Menella, V. and Mottola, S. and Neukum, G. and Orofino, V. and Palumbo, P. and Piccioni, G. and Rauer, H. and Schmitt, B. and Tiphene, D. and Taylor, F. W. and Tozzi, G. P. (2010) Martian atmosphere as observed by VIRTIS-M on Rosetta spacecraft. Journal of Geophysical Research, 115 (E4), E04004. DOI: 10.1029/2009JE003345. ISSN 0148-0227.
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The Rosetta spacecraft accomplished a flyby of Mars on its way to 67P/Churyumov-Gerasimenko on 25 February 2007. In this paper we describe the measurements obtained by the M channel of the Visual and Infrared Thermal Imaging Spectrometer (VIRTIS-M) and the first scientific results derived from their analysis. The broad spectral coverage of the VIRTIS-M in the IR permitted the study of various phenomena occurring in the Martian atmosphere; observations were further exploited to achieve accurate absolute radiometric calibration. Nighttime data from the VIRTIS-M constrain the air temperature profile in the lower atmosphere (5-30 km), using variations in CO2 opacity at 4.3 μm. A comparison of this data with the global circulation model (GCM) by Forget et al. (1999) shows a trend of slightly higher air temperature in the VIRTIS-M retrievals; this is accompanied by the presence of moderate decreases (˜5 K) in large sections of the equatorial region. This is potentially related to the occurrence of water ice clouds. Daytime data from the VIRTIS-M reveal CO2 non-local thermodynamic equilibrium emission in the high atmosphere. A mapping of emission intensity confirms its strict dependence on solar zenith angle. Additionally, devoted limb observations allowed the retrieval of vertical emission intensity profiles, indicating a peak around 105 km in southern tropical regions. Ozone content can be effectively monitored by the emission of O2 (a1Δg) at 1.27 μm. Retrieved emission intensity shows that polar regions are particularly rich in ozone. Aerosol scattering was observed in the 1-2.5 μm region above the night region above the night disk, suggesting the occurrence of very high noctilucent clouds.
|Title:||Martian atmosphere as observed by VIRTIS-M on Rosetta spacecraft|
|Journal or Publication Title:||Journal of Geophysical Research|
|In Open Access:||No|
|In ISI Web of Science:||Yes|
|Keywords:||Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Instruments and techniques, Planetary Sciences: Solid Surface Planets: Remote sensing|
|HGF - Research field:||Aeronautics, Space and Transport (old)|
|HGF - Program:||Space (old)|
|HGF - Program Themes:||W EW - Erforschung des Weltraums|
|DLR - Research area:||Space|
|DLR - Program:||W EW - Erforschung des Weltraums|
|DLR - Research theme (Project):||W - Projekt ROSETTA Instrumente (old)|
|Institutes and Institutions:||Institute of Planetary Research > Asteroids and Comets|
Institute of Planetary Research > Extrasolar Planets and Atmospheres
|Deposited By:||Laura-Maria Brumm|
|Deposited On:||02 Nov 2010 10:36|
|Last Modified:||23 Jan 2014 11:36|
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