KEPLER'S SUPERNOVA: AN OVERLUMINOUS TYPE Ia EVENT INTERACTING with A MASSIVE CIRCUMSTELLAR MEDIUM at A VERY LATE PHASE

Satoru Katsuda, Koji Mori, Keiichi Maeda, Masaomi Tanaka, Katsuji Koyama, Hiroshi Tsunemi, Hiroshi Nakajima, Yoshitomo Maeda, Masanobu Ozaki, Robert Petre

研究成果: Article査読

28 被引用数 (Scopus)

抄録

We have analyzed XMM-Newton, Chandra, and Suzaku observations of three similarly aged, ejecta-dominated supernova remnants (SNRs), Kepler's SNR, Tycho's SNR, and SNR 0509-67.5, to investigate the properties of the SN ejecta and the circumstellar medium (CSM). By simply comparing the X-ray spectra, we find that line intensity ratios of iron-group elements (IGEs) to intermediate-mass elements (IMEs) for Kepler's SNR and SNR 0509-67.5 are much higher than those for Tycho's SNR. Given that Tycho's SNR and SNR 0509-67.5 are thought to be the remnants of a typical SN Ia and an overluminous SN Ia, respectively, we argue that Kepler is the product of an overlumious SN Ia. This inference is supported by our spectral modeling, which reveals the IGE and IME masses, respectively, to be and (Kepler's SNR), and (SNR 0509-67.5), and and (Tycho's SNR). We find that the CSM component in Kepler's SNR consists of tenuous diffuse gas (∼0.3 ) present throughout the entire remnant, plus dense knots (∼0.035 ). Since both of them show N overabundance, their origin would be CNO-processed material from the progenitor system. The mass of the diffuse CSM allows us to infer the pre-SN mass-loss rate to be (vw/10 km s-1) yr-1. The dense knots have slow proper motions and relatively small ionization timescales; hence, they were likely located a few parsecs away from the progenitor at the explosion. We thus argue that Kepler's SN was an overluminous (91T-like) event that recently started to interact with the massive CSM. This supports the possible link between 91T-like SNe and "Ia-CSM" SNe.

本文言語English
論文番号49
ジャーナルAstrophysical Journal
808
1
DOI
出版ステータスPublished - 2015 7 20
外部発表はい

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学

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