EVIDENCE FOR THERMAL X-RAY LINE EMISSION FROM THE SYNCHROTRON-DOMINATED SUPERNOVA REMNANT RX J1713.7-3946

被引：41

作者：

Katsuda, Satoru ^{[1
]}

Acero, Fabio ^{[2
]}

Tominaga, Nozomu ^{[3
,4
]}

Fukui, Yasuo ^{[5
]}

Hiraga, Junko S. ^{[6
]}

Koyama, Katsuji ^{[7
,8
]}

Lee, Shiu-Hang ^{[1
]}

Mori, Koji ^{[9
]}

Nagataki, Shigehiro ^{[10
]}

Ohira, Yutaka ^{[11
]}

Petre, Robert ^{[12
]}

Sano, Hidetoshi ^{[5
,13
]}

Takeuchi, Yoko ^{[13
]}

Tamagawa, Toru ^{[13
]}

Tsuji, Naomi ^{[14
]}

Tsunemi, Hiroshi ^{[7
]}

Uchiyama, Yasunobu ^{[14
]}

机构：

[1] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan

[2] Univ Paris Diderot, Lab AIM, Serv Astrophys,CEA Saclay, CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France

[3] Konan Univ, Fac Sci & Engn, Dept Phys, Kobe, Hyogo 6588501, Japan

[4] Univ Tokyo, Kav li Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

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

[6] Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, Sanda 6691337, Japan

[7] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

[8] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan

[9] Miyazaki Univ, Fac Engn, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan

[10] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan

[11] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan

[12] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

[13] Nagoya Univ, Inst Adv Res, Chikusa Ku, Nagoya, Aichi 4648601, Japan

[14] RIKEN, Nishina Ctr, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 814卷 / 01期

基金：

日本学术振兴会;

关键词：

ISM: individual objects (RX J1713.7-3946); ISM: supernova remnants; supernovae: general; X-rays: general; TEV GAMMA-RAY; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; SHOCK ACCELERATION; INTERSTELLAR GAS; UBVRI PHOTOMETRY; STARS; NUCLEOSYNTHESIS; SHELL; RX-J1713.7-3946;

D O I：

10.1088/0004-637X/814/1/29

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the first detection of thermal X-ray line emission from the supernova remnant (SNR) RX J1713.7-3946, the prototype of the small class of synchrotron-dominated SNRs. A softness-ratio map generated using XMM-Newton data shows that faint interior regions are softer than bright shell regions. Using Suzaku and deep XMM-Newton observations, we have extracted X-ray spectra from the softest area, finding clear line features at E-ph similar to 1 and similar to 1.35 keV. These lines can be best explained as Ne Lya and Mg Heck from a thermal emission component. Since the abundance ratios of metals to Fe are much higher than solar values in the thermal component, we attribute the thermal emission to reverse-shocked SN ejecta. The measured Mg/Ne, Si/Ne, and Fe/Ne ratios of 2.0-2.6, 1.5-2.0, and <0.05 solar suggest that the progenitor star of RX J1713.7-3946 was a relatively low-mass star (less than or similar to 20 M-circle dot), consistent with a previous inference based on the effect of stellar winds of the progenitor star on the surrounding medium. Since the mean blastwave speed of similar to 6000 km s(-1) (the radius of 9.6 pc divided by the age of 1600 years) is relatively fast compared with other core-collapse SNRs, we propose that RX J1713.7-3946 is a result of an SN Ib/c whose progenitor was a member of an interacting binary. While our analysis provides strong evidence for X-ray line emission, our interpretation of its nature as thermal emission from SN ejecta requires further confirmation especially through future precision spectroscopic measurements using ASTRO-H.

引用

页数：11

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