Reference : Measurements of the helium 584 Å airglow during the Cassini flyby of Venus
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/100142
Measurements of the helium 584 Å airglow during the Cassini flyby of Venus
English
Gérard, Jean-Claude mailto [Laboratoire de Physique Atmosphérique et Planétaire, Université de Liège, 17, allée du 6 août, B5c, B-4000 Liège, Belgium]
Gustin, Jacques mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP)]
Hubert, Benoît mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP)]
Gladstone, G. R. [Southwest Research Institute, P.O. Drawer 28510, 6220 Culebra Road, San Antonio, TX 78238-5166, USA]
Esposito, L. W. [Laboratory for Atmospheric and Space Physics, University of Colorado, Campus Box 392, Boulder, CO 80309-0392, USA]
1-Oct-2011
Planetary and Space Science
Pergamon Press - An Imprint of Elsevier Science
59
1524-1528
Yes (verified by ORBi)
International
0032-0633
Oxford
United Kingdom
[en] The helium resonance line at 584 Å has been observed with the UltraViolet Imaging Spectrograph (UVIS) Extreme Ultraviolet channel during the flyby of Venus by Cassini at a period of high solar activity. The brightness was measured along the disk from the morning terminator up to the bright limb near local noon. The mean disk intensity was ˜320 R, reaching ˜700 R at the bright limb. These values are slightly higher than those determined from previous observations. The sensitivity of the 584 Å intensity to the helium abundance is analyzed using recent cross-sections and solar irradiance measurements at 584 Å. The intensity distribution along the UVIS footprint on the disk is best reproduced using the EUVAC solar flux model and the helium density distribution from the VTS3 empirical model. It corresponds to a helium density of 8×10[SUP]6[/SUP] cm[SUP]-3[/SUP] at the level of where the CO[SUB]2[/SUB] is 2×10[SUP]10[/SUP] cm[SUP]-3[/SUP].
Researchers ; Professionals
http://hdl.handle.net/2268/100142
10.1016/j.pss.2011.06.018
http://adsabs.harvard.edu/abs/2011P%26SS...59.1524G

File(s) associated to this reference

Fulltext file(s):

FileCommentaryVersionSizeAccess
Open access
UVIS-EUV_final.pdfAuthor preprint1.21 MBView/Open

Bookmark and Share SFX Query

All documents in ORBi are protected by a user license.