Reference : Simultaneous Cassini VIMS and UVIS observations of Saturn's southern aurora
Scientific congresses and symposiums : Paper published in a book
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/128407
Simultaneous Cassini VIMS and UVIS observations of Saturn's southern aurora
English
Melin, H. [Department of Physics & Astronomy, University of Leicester, United Kingdom (h.melin@ion.le.ac.uk); Space Environment Technologies, Planetary and Space Science Division, Pacific Palisades, United States (h.melin@gmail.com)]
Stallard, T. [Department of Physics & Astronomy, University of Leicester, United Kingdom (h.melin@ion.le.ac.uk)]
Miller, S. [University College London, UK]
Gustin, Jacques mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Physique des atmosphères et des environnements planétaires >]
Galand, M. [Imperial College, UK]
Badman, S. V. [JAXA Institute of Space and Astronautical Science, Japan]
Pryor, W. [Space Environment Technologies, Planetary and Space Science Division, Pacific Palisades, United States (h.melin@gmail.com); Central Arizona College, USA]
O'Donoghue, J. [Department of Physics & Astronomy, University of Leicester, United Kingdom (h.melin@ion.le.ac.uk)]
Brown, R. H. [University of Arizona, USA]
Baines, K. H. [)]
1-Oct-2011
EPSC-DPS Joint Meeting 2011
1764
No
EPSC-DPS Joint Meeting 2011
2-7 October 2011
[en] Here, temporally simultaneous and spatially overlapping Cassini VIMS and UVIS observations of Saturn's southern aurora are presented. The pointing is fixed at a constant local time of 04:55, covering latitudes between 64°S and 82°S and longitudes between 127° and 186°. The spatial resolution is high, with 1 mrad covering ˜300 km, such that only a small part of the pre-dawn aurora is observed. Ultraviolet auroral H and H2 emissions from UVIS are compared to infrared H+3 emission from VIMS. The auroral emission is structured into three arcs - H, H2 and H+3 are morphologically identical in the bright main auroral oval (˜73°S), but there is an equatorward arc that is seen predominantly in H (˜70°S), and a poleward arc (˜74°S) that is seen mainly in H2 and H+3 . These observations indicate that, for the main auroral oval, the UV emission is a good proxy for the infrared H+3 morphology (and vice versa), but for emission either poleward or equatorward this is no longer true. Hence, given the highly dynamic nature of the aurora of Saturn, simultaneous UV/IR observations are crucial for completing the picture of how the atmosphere interacts with the magnetosphere.
http://hdl.handle.net/2268/128407
http://adsabs.harvard.edu/abs/2011epsc.conf.1764M

There is no file associated with this reference.

Bookmark and Share SFX Query

All documents in ORBi are protected by a user license.