Reference : Auroral and Non-auroral X-ray Emissions from Jupiter: A Comparative View
Scientific congresses and symposiums : Poster
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/97486
Auroral and Non-auroral X-ray Emissions from Jupiter: A Comparative View
English
Bhardwaj, A. [> > > >]
Elsner, R. [> > > >]
Gladstone, R. [> > > >]
Waite, H. [> > > >]
Lugaz, N. [> > > >]
Cravens, T. [> > > >]
Branduardi-Raymont, G. [> > > >]
Ramsay, G. [> > > >]
Soria, R. [> > > >]
Ford, P. [> > > >]
Rodriguez, P. [> > > >]
Majeed, T. [> > > >]
Grodent, Denis mailto [ > > ]
2004
No
No
International
American Geophysical Union Fall Meeting 2004
13-17 December, 2004
San Francisco
CA
[en] 7554 X rays ; gamma rays ; and neutrinos ; 6220 Jupiter ; 2455 Particle precipitation ; 0310 Airglow and aurora ; 0343 Planetary atmospheres (5405 ; 5407 ; 5409 ; 5704 ; 5705 ; 5707)
[en] Jovian X-rays can be broadly classified into two categories: (1) "auroral" emission, which is confined to high-latitudes ( ˜>60° ) at both polar regions, and (2) "dayglow" emission, which originates from the sunlit low-latitude ( ˜<50° ) regions of the disk (hereafter called "disk" emissions). Recent X-ray observations of Jupiter by Chandra and XMM-Newton have shown that these two types of X-ray emission from Jupiter have different morphological, temporal, and spectral characteristics. In particular: 1) contrary to the auroral X-rays, which are concentrated in a spot in the north and in a band that runs half-way across the planet in the south, the low-latitude X-ray disk is almost uniform; 2) unlike the ˜40±20-min periodic oscillations seen in the auroral X-ray emissions, the disk emissions do not show any periodic oscillations; 3) the disk emission is harder and extends to higher energies than the auroral spectrum; and 4) the disk X-ray emission show time variability similar to that seen in solar X-rays. These differences and features imply that the processes producing X-rays are different at these two latitude regions on Jupiter. We will present the details of these and other features that suggest the differences between these two classes of X-ray emissions from Jupiter, and discuss the current scenario of the production mechanism of them.
http://hdl.handle.net/2268/97486
also: http://hdl.handle.net/2268/94014
http://www.agu.org/meetings/fm04/

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