Reference : A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/29723
A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express
English
Drossart, P. [> > > >]
Piccioni, G. [> > > >]
Gérard, Jean-Claude mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]
Lopez-Valverde, M. A. [> > > >]
Sanchez-Lavega, A. [> > > >]
Zasova, L. [> > > >]
Hueso, R. [> > > >]
Taylor, F. W. [> > > >]
Bezard, B. [> > > >]
Adriani, A. [> > > >]
Angrilli, F. [> > > >]
Arnold, G. [> > > >]
Baines, K. H. [> > > >]
Bellucci, G. [> > > >]
Benkhoff, J. [> > > >]
Bibring, J. P. [> > > >]
Blanco, A. [> > > >]
Blecka, M. I. [> > > >]
Carlson, R. W. [> > > >]
Coradini, A. [> > > >]
Di Lellis, A. [> > > >]
Encrenaz, T. [> > > >]
Erard, S. [> > > >]
Fonti, S. [> > > >]
Formisano, V. [> > > >]
Fouchet, T. [> > > >]
Garcia, R. [> > > >]
Haus, R. [> > > >]
Helbert, J. [> > > >]
Ignatiev, N. I. [> > > >]
Irwin, P. [> > > >]
Langevin, Y. [> > > >]
Lebonnois, S. [> > > >]
Luz, D. [> > > >]
Marinangeli, L. [> > > >]
Orofino, V. [> > > >]
Rodin, A. V. [> > > >]
Roos-Serote, M. C. [> > > >]
Saggin, B. [> > > >]
Stam, D. M. [> > > >]
Titov, D. [> > > >]
Visconti, G. [> > > >]
Zambelli, M. [> > > >]
Tsang, C. [> > > >]
VIRTIS-Venus Express Tech, Te [> > > >]
2007
Nature
Nature Publishing Group
450
641-645
Yes (verified by ORBi)
International
0028-0836
1476-4687
Basingstoke
United Kingdom
[en] Venus ; airglow ; oxygen
[en] The upper atmosphere of a planet is a transition region in which energy is transferred between the deeper atmosphere and outer space. Molecular emissions from the upper atmosphere (90-120 km altitude) of Venus can be used to investigate the energetics and to trace the circulation of this hitherto little-studied region. Previous spacecraft(1) and ground-based(2-4) observations of infrared emission from CO2, O-2 and NO have established that photochemical and dynamic activity controls the structure of the upper atmosphere of Venus. These data, however, have left unresolved the precise altitude of the emission(1) owing to a lack of data and of an adequate observing geometry(5,6). Here we report measurements of day-side CO2 non-local thermodynamic equilibrium emission at 4.3 mu m, extending from 90 to 120 km altitude, and of night-side O-2 emission extending from 95 to 100 km. The CO2 emission peak occurs at similar to 115 km and varies with solar zenith angle over a range of similar to 10 km. This confirms previous modelling(7), and permits the beginning of a systematic study of the variability of the emission. The O-2 peak emission happens at 96 km +/- 1 km, which is consistent with three-body recombination of oxygen atoms transported from the day side by a global thermospheric sub-solar to anti-solar circulation, as previously predicted(8).
Researchers ; Professionals
http://hdl.handle.net/2268/29723
also: http://hdl.handle.net/2268/2714
10.1038/nature06140

File(s) associated to this reference

Fulltext file(s):

FileCommentaryVersionSizeAccess
Restricted access
drossart_2007_a dynamic.pdfNo commentaryPublisher postprint1.49 MBRequest copy

Bookmark and Share SFX Query

All documents in ORBi are protected by a user license.