HR: 0800h
AN: P51B-1432    [Abstracts]
TI: Auroral and Non-auroral X-ray Emissions from Jupiter: A Comparative View
AU: * Bhardwaj, A
EM: Anil.Bhardwaj@msfc.nasa.gov
AF: NASA Marshall Space Flight Center, NSSTC/SD50, 320 Sparkman Drive, Huntsville, AL 35805 United States
AU: Elsner, R
EM: ron.elsner@msfc.nasa.gov
AF: NASA Marshall Space Flight Center, NSSTC/SD50, 320 Sparkman Drive, Huntsville, AL 35805 United States
AU: Gladstone, R
EM: randy.gladstone@swri.org
AF: Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228 United States
AU: Waite, H
EM: hunterw@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109 United States
AU: Lugaz, N
EM: nlugaz@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109 United States
AU: Cravens, T
EM: cravens@ku.edu
AF: University of Kansas, 1251 Wescoe Hall Dr., Lawrence, KS 66045 United States
AU: Branduardi-Raymont, G
EM: gbr@mssl.ucl.ac.uk
AF: University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Ramsay, G
EM: gtbr@mssl.ucl.ac.uk
AF: University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Soria, R
EM: rs1@mssl.ucl.ac.uk
AF: University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Ford, P
EM: pgf@space.mit.edu
AF: Massachusetts Institute of Technology, 37-635, 70 Vassar Street, Cambridge, MA 02139 United States
AU: Rodriguez, P
EM: prodrigu@xmm.vilspa.esa.es
AF: XMM-Newton SOC, Apartado 50727, Villafranca, Madrid, 28080 Spain
AU: Majeed, T
EM: tariqm@engin.umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109 United States
AU: Grodent, D
EM: d.grodent@ulg.ac.be
AF: LPAP, Universite de Liege, Liege, B-4000 Belgium
AB: Jovian X-rays can be broadly classified into two categories: (1) "auroral" emission, which is confined to high-latitudes ($\sim>60\deg$) at both polar regions, and (2) "dayglow" emission, which originates from the sunlit low-latitude ($\sim<50\deg$) 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 $\sim40\pm20$-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.
DE: 7554 X rays, gamma rays, and neutrinos
DE: 6220 Jupiter
DE: 2455 Particle precipitation
DE: 0310 Airglow and aurora
DE: 0343 Planetary atmospheres (5405, 5407, 5409, 5704, 5705, 5707)
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting