XMM-Newton observations of X-ray emission from Jupiter

被引：0

作者：

Branduardi-Raymont, G ^{[1
]}

Bhardwaj, A

Elsner, RF

Gladstone, GR

Ramsay, G

Rodriguez, P

Soria, R

Waite, JH

Cravens, TE

机构：

[1] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[2] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India

[3] NASA, Marshall Space Flight Ctr, NSSTC XD12, Huntsville, TX 35805 USA

[4] Southwest Res Inst, San Antonio, TX 78228 USA

[5] XMM NewtonSOC, Madrid 28080, Spain

[6] Univ Michigan, Ann Arbor, MI 48109 USA

[7] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

来源：

PROCEEDINGS OF THE X-RAY UNIVERSE 2005, VOLS 1 AND 2 | 2006年 / 604卷

关键词：

planets; Jupiter; X-rays;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of two XMM-Newton observations of Jupiter carried out in 2003 for 100 and 250 ks (or 3 and 7 planet rotations) respectively. X-ray images from the EPIC CCD cameras show prominent emission from the auroral regions in the 0.2-2.0 keV band: the spectra are well modelled by a combination of emission lines, including most prominently those of highly ionised oxygen (OVIII and OVIII). In addition, and for the first time, XMM-Newton reveals the presence in both aurorae of a higher energy component (3-7 keV) which is well described by an electron bremsstrahlung spectrum. This component is found to be variable in flux and spectral shape during the Nov. 2003 observation, which corresponded to an extended period of intense solar activity. Emission from the equatorial regions of the Jupiter's disk is also observed, with a spectrum consistent with that of solar X-rays scattered in the planet's upper atmosphere. Jupiter's X-rays are spectrally resolved with the RGS which clearly separates the prominent OVII contribution of the aurorae from the OVIII, FeXVII and MgXI lines, originating in the low-latitude disk regions of the planet.

引用

页码：15 / +

页数：2

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