2015年11月
Evidence for Thermal X-Ray Line Emission from the Synchrotron-dominated Supernova Remnant RX J1713.7-3946
The Astrophysical Journal
- 巻
- 814
- 号
- 1
- 記述言語
- 英語
- 掲載種別
- 研究論文(学術雑誌)
- DOI
- 10.1088/0004-637X/814/1/29
- 出版者・発行元
- IOP PUBLISHING LTD
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 } }∼ 1 and ∼1.35 keV. These lines can be best explained as Ne Lyα and Mg Heα 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 (≲20 M☉), 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 ∼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....
- リンク情報
- ID情報
-
- DOI : 10.1088/0004-637X/814/1/29
- ISSN : 0004-637X
- eISSN : 1538-4357
- ORCIDのPut Code : 77153058
- arXiv ID : arXiv:1510.04025
- Web of Science ID : WOS:000365310200029
- BibTex Code : 2015ApJ...814...29K