Suzaku observations of Jovian diffuse hard X-ray emission

被引:1
|
作者
Numazawa, Masaki [1 ]
Ezoe, Yuichiro [1 ]
Ohashi, Takaya [1 ]
Ishikawa, Kumi [2 ]
Miyoshi, Yoshizumi [3 ]
Shiota, Daikou [3 ,4 ]
Uchiyama, Yasunobu [5 ]
Kimura, Tomoki [6 ]
Branduardi-Raymont, Graziella [7 ]
机构
[1] Tokyo Metropolitan Univ, Dept Phys, 1-1 Minami Osawa, Hachioji, Tokyo 1920397, Japan
[2] Japan Aerosp & Explorat Agcy JAXA, Inst Space & Astronaut Sci ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan
[3] Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan
[4] Natl Inst Informat & Commun Technol, Appl Electromagnet Res Inst, 4-2-1 Nukui Kita, Koganei, Tokyo 1848795, Japan
[5] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan
[6] Tohoku Univ, Dept Geophys, Aoba Ku, 6-3 Aramaki, Sendai, Miyagi 9808578, Japan
[7] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
基金
日本学术振兴会;
关键词
planets and satellites: general; planets and satellites: individual (Jupiter); X-rays: general; PHOTON IMAGING CAMERA; XMM-NEWTON; JUPITER; PRECIPITATION; ELECTRONS;
D O I
10.1093/pasj/psab053
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report on results of systematic analyses of the entire three X-ray data sets of Jupiter taken by Suzaku in 2006, 2012, and 2014. Jovian diffuse hard X-ray emission was discovered by Suzaku in 2006 when the solar activity went toward its minimum. The diffuse emission was spatially consistent with the Jovian inner magnetosphere and was spectrally fitted with a flat power-law function suggesting non-thermal emission. Thus, a scenario in which ultra-relativistic (tens of MeV) electrons in the Jovian inner magnetosphere inverse-Comptonize solar visible photons into X-ray bands has been hypothetically proposed. We focused on the dependence of the Jovian diffuse hard X-ray emission on the solar activity to verify this scenario. The solar activity in 2012 and 2014 was around the maximum of the 24th solar cycle. By combining the imaging and spectral analyses for the three data sets, we successfully separated the contribution of the diffuse emission from the emission of Jupiter's body (i.e., the aurora and disk emission). The 1-5 keV luminosity of the diffuse emission has been stable and did not vary significantly, and did not simply depend on the solar activity, which is also known to affect the high-energy electron distribution in the Jovian inner magnetosphere scarcely. The luminosity of the body emission both in 0.2-1 and 1-5 keV, in contrast, probably depended on the solar activity and varied by a factor of 2-5. These results strongly supported the inverse-Compton scattering scenario by the ultra-relativistic electrons. In this paper, we estimate spatial and spectral distributions of the inverse-Compton scattering X-rays by Jovian magneto-spheric high-energy electrons with reference to the Divine-Garrett model and found a possible agreement in an inner region (less than or similar to 10 R-J) for the X-ray observations.
引用
收藏
页码:894 / 911
页数:18
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