NON-THERMAL X-RAYS AND INTERSTELLAR GAS TOWARD THE γ-RAY SUPERNOVA REMNANT RX J1713.7-3946: EVIDENCE FOR X-RAY ENHANCEMENT AROUND CO AND H I CLUMPS

被引：41

作者：

Sano, H. ^{[1
]}

Tanaka, T. ^{[2
]}

Torii, K. ^{[1
]}

Fukuda, T. ^{[1
]}

Yoshiike, S. ^{[1
]}

Sato, J. ^{[1
]}

Horachi, H. ^{[1
]}

Kuwahara, T. ^{[1
]}

Hayakawa, T. ^{[1
]}

Matsumoto, H. ^{[1
]}

Inoue, T. ^{[3
]}

Yamazaki, R. ^{[3
]}

Inutsuka, S. ^{[1
]}

Kawamura, A. ^{[1
,4
]}

Tachihara, K. ^{[1
]}

Yamamoto, H. ^{[1
]}

Okuda, T. ^{[1
]}

Mizuno, N. ^{[1
,4
]}

Onishi, T. ^{[1
,5
]}

Mizuno, A. ^{[6
]}

Fukui, Y. ^{[1
]}

机构：

[1] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648601, Japan

[2] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan

[3] Aoyama Gakuin Univ, Dept Math & Phys, Chuou Ku, Sagamihara, Kanagawa 2525258, Japan

[4] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[5] Osaka Prefecture Univ, Grad Sch Sci, Dept Astrophys, Naka Ku, Sakai, Osaka 5998531, Japan

[6] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 778卷 / 01期

基金：

日本学术振兴会;

关键词：

cosmic rays; ISM: clouds; ISM: individual objects (RX J1713.7-3946); ISM: supernova remnants; X-rays: ISM; GALACTIC PLANE SURVEY; COSMIC-RAYS; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; MAGNETIC-FIELD; XMM-NEWTON; SHELL; TEV; HESS; G347.3-0.5;

D O I：

10.1088/0004-637X/778/1/59

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

RX J1713.7-3946 is the most remarkable very high energy gamma-ray supernova remnant that emits synchrotron X-rays without thermal features. We made a comparative study of CO, Hi, and X-rays in order to better understand the relationship between the X-rays, and the molecular and atomic gas. The results indicate that the X-rays are enhanced around the CO and H I clumps on a pc scale, but are decreased inside the clumps on a 0.1 pc scale. Magnetohydrodynamic numerical simulations of the shock interaction with molecular and atomic gas indicate that the interaction between the shock waves and the clumps excite turbulence, which amplifies the magnetic field around the clumps. We suggest that the amplified magnetic field around the CO and H I clumps enhances the synchrotron X-rays and possibly the acceleration of cosmic-ray electrons.

引用

页数：19

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