HR: 15:45h
AN: P44A-02    [Abstracts]
TI: X-ray Emissions from Jupiter as Observed with XMM-Newton
AU: * Branduardi-Raymont, G
EM: gbr@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Bhardwaj, A
EM: Anil.Bhardwaj@msfc.nasa.gov
AF: NASA Marshall Space Flight Center Space Science Branch, XD12, National Space Science and Technology Center 320 Sparkman Drive, Huntsville, AL 35805 United States
AU: Elsner, R F
EM: ron.elsner@msfc.nasa.gov
AF: NASA Marshall Space Flight Center Space Science Branch, XD12, National Space Science and Technology Center 320 Sparkman Drive, Huntsville, AL 35805 United States
AU: Gladstone, G R
EM: randy.gladstone@swri.org
AF: Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228-0510 United States
AU: Ramsay, G
EM: gtbr@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Rodriguez, P
EM: pedro.rodriguez@sciops.esa.int
AF: XMM-Newton SOC, Apartado 50727 Villafranca, Madrid, 28080 Spain
AU: Soria, R
EM: rs1@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT United Kingdom
AU: Waite, J H
EM: hunterw@umich.edu
AF: Department of Atmospheric, Oceanic, and Space Sciences The University of Michigan, Space Research Building 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Cravens, T E
EM: cravens@mail.ku.edu
AF: Department of Physics and Astronomy University of Kansas, 1251 Wescoe Hall Dr., Lawrence, KS 66045 United States
AB: We present two XMM-Newton observations of Jupiter, which were carried out in April and November 2003 for 110 and 250 ks (or 3 and 7 planet rotations) respectively. X-ray images taken with XMM-Newton EPIC CCD cameras show prominent emission, essentially all confined to the 0.2 - 2.0 keV band, from Jupiter's auroral spots; their spectra can be modelled with a combination of unresolved emission lines, including most prominently those of highly ionised oxygen (OVII and OVIII). Emission from the equatorial regions of the planet's disk is also observed. Its spectrum is consistent with that of solar X-rays scattered in the planet's upper atmosphere. More remarkably, we find that in November 2003 a large solar X-ray flare, taking place on the Sun's Jupiter-facing side, is associated with a corresponding feature in the Jovian X-ray lightcurve of the equatorial regions. Jupiter's X-ray emissions are spectrally resolved with XMM-Newton Reflection Grating Spectrometer (RGS). The high energy resolution provided by RGS allows us to clearly separate the OVII and OVIII lines in the spectra, and to identify most of the auroral emission with the lower ionisation line. The North auroral spot emission is deeply modulated at the planet's rotation period. Moreover, the X-ray emission from Jupiter's disk displays prominent line contribution due to FeXVII, in addition to an OVIII component. Our temporal and spectral findings suggest that the non-auroral X-ray emission from Jupiter is directly controlled by the Sun. On the other hand, the spectral results presented here support the hypothesis that Jupiter's auroral emissions originate from the capture and acceleration of solar wind ions in the planet's magnetosphere, followed by X-ray production by charge exchange.
DE: 2164 Solar wind plasma
DE: 2704 Auroral phenomena (2407)
DE: 6220 Jupiter
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
SC: Planetary Sciences [P]
MN: 2005 Joint Assembly