Latest results on Jovian disk X-rays from XMM-Newton |
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| Affiliation: | 1. Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK;2. Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum 695022, India;3. NASA Marshall Space Flight Center, NSSTC/XD12, 320 Sparkman Drive, Huntsville, AL 35805, USA;4. Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX 78228, USA;5. XMM-Newton SOC, Apartado 50727, Villafranca, 28080 Madrid, Spain;6. University of Michigan, Space Research Building, 2455 Hayward, Ann Arbor, MI 48109, USA;7. Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA;1. Observatoire de Paris-Meudon, France;2. Vikram Sarabhai Space Centre, Trivandrum, India;3. National Central University, Jhongli City, Taiwan (ROC);1. Department of Mechanical Nuclear and Production Engineering, University of Pisa, Italy;2. Sogin Spa, Caorso Nuclear Power Plant, Italy;1. Department of Science, Natural Resources and Outdoor Studies, University of Cumbria, Bowerham Road LA1 3JD, United Kingdom;2. Department of Engineering, Lancaster University, Bailrigg LA1 4YR, United Kingdom;1. University of Tartu, Institute of Physics, Riia 142, 51014 Tartu, Estonia;2. Tallinn University of Technology, Department of Chemical Engineering, Ehitajate tee 5, 19086 Tallinn, Estonia |
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| Abstract: | We present the results of a spectral study of the soft X-ray emission (0.2–2.5 keV) from low-latitude (‘disk’) regions of Jupiter. The data were obtained during two observing campaigns with XMM-Newton in April and November 2003. While the level of the emission remained approximately the same between April and the first half of the November observation, the second part of the latter shows an enhancement by about 40% in the 0.2–2.5 keV flux. A very similar, and apparently correlated increase, in time and scale, was observed in the solar X-ray and EUV flux.The months of October and November 2003 saw a period of particularly intense solar activity, which appears reflected in the behavior of the soft X-rays from Jupiter's disk. The X-ray spectra, from the XMM-Newton EPIC CCD cameras, are all well fitted by a coronal model with temperatures in the range 0.4–0.5 keV, with additional line emission from Mg XI (1.35 keV) and Si XIII (1.86 keV): these are characteristic lines of solar X-ray spectra at maximum activity and during flares.The XMM-Newton observations lend further support to the theory that Jupiter's disk X-ray emission is controlled by the Sun, and may be produced in large part by scattering, elastic and fluorescent, of solar X-rays in the upper atmosphere of the planet. |
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