Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite

Kimura T.; Kraft R. P.; Elsner R. F.Branduardi-Raymont G.Gladstone G. R.Tao C.Yoshioka K.Murakami G.Yamazaki A.Tsuchiya F.Vogt M. F.Masters A.Hasegawa H.Badman S. V.Roediger E.Ezoe Y.Dunn W. R.Yoshikawa I.Fujimoto M.Murray S. S.

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Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite

机译：Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite

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abstract_textpJupiter's X-ray auroral emission in the polar cap region results from particles which have undergone strong field-aligned acceleration into the ionosphere. The origin of precipitating ions and electrons and the time variability in the X-ray emission are essential to uncover the driving mechanism for the high-energy acceleration. The magnetospheric location of the source field line where the X-ray is generated is likely affected by the solar wind variability. However, these essential characteristics are still unknown because the long-term monitoring of the X-rays and contemporaneous solar wind variability has not been carried out. In April 2014, the first long-term multiwavelength monitoring of Jupiter's X-ray and EUV auroral emissions was made by the Chandra X-ray Observatory, XMM-Newton, and Hisaki satellite. We find that the X-ray count rates are positively correlated with the solar wind velocity and insignificantly with the dynamic pressure. Based on the magnetic field mapping model, a half of the X-ray auroral region was found to be open to the interplanetary space. The other half of the X-ray auroral source region is magnetically connected with the prenoon to postdusk sector in the outermost region of the magnetosphere, where the Kelvin-Helmholtz (KH) instability, magnetopause reconnection, and quasiperiodic particle injection potentially take place. We speculate that the high-energy auroral acceleration is associated with the KH instability and/or magnetopause reconnection. This association is expected to also occur in many other space plasma environments such as Saturn and other magnetized rotators./p/abstract_text

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《Journal of geophysical research》 |2016年第3期|2308-2320|共13页
作者
Kimura T.; Kraft R. P.; Elsner R. F.Branduardi-Raymont G.Gladstone G. R.Tao C.Yoshioka K.Murakami G.Yamazaki A.Tsuchiya F.Vogt M. F.Masters A.Hasegawa H.Badman S. V.Roediger E.Ezoe Y.Dunn W. R.Yoshikawa I.Fujimoto M.Murray S. S.;
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Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan;

RIKEN, Nishina Ctr Accelerator Based Sci, Saitama, Japan;

Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USANASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USAUniv Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, EnglandSW Res Inst, Dept Space Studies, Boulder, CO USAUniv Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, FranceTohoku Univ, Planetary Plasma & Atmospher Res Ctr, Sendai, Miyagi 980, JapanBoston Univ, Ctr Space Phys, Boston, MA 02215 USAUniv London Imperial Coll Sci Technol & Med, Dept Phys, Fac Nat Sci, London, EnglandUniv Lancaster, Dept Phys, Lancaster, EnglandUniv Hamburg, Hamburger Sternwarte, Hamburg, GermanyTokyo Metropolitan Univ, Tokyo 158, JapanUniv Tokyo, Dept Complex Sci & Engn, Chiba, JapanTokyo Inst Technol, Earth Life Sci Inst, Tokyo 152, Japan;

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Jupiter; X-ray; magnetosphere; KELVIN-HELMHOLTZ VORTICES; PHOTON IMAGING CAMERA; SOLAR-WIND; RELATIVISTIC ELECTRONS; SATURNS MAGNETOPAUSE; MAGNETIC-FIELD; ULYSSES RADIO; MAGNETOSPHERE; EMISSION; BURSTS;

Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite

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