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アキタヤ ヒロシ
秋田谷 洋 所属 千葉工業大学 天文学研究センター 天文学研究センター 職種 上席研究員 |
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| 言語種別 | 英語 |
| 発行・発表の年月 | 2018/12/01 |
| 形態種別 | 学術雑誌 |
| 標題 | Extended optical/NIR observations of Type Iax supernova 2014dt: Possible signatures of a bound remnant |
| 執筆形態 | 共著 |
| 掲載誌名 | Publications of the Astronomical Society of Japan |
| 掲載区分 | 国外 |
| 出版社・発行元 | Oxford University Press (OUP) |
| 巻・号・頁 | 70(6),pp.111 |
| 著者・共著者 | Miho Kawabata, Koji S Kawabata, Keiich Maeda, Masayuki Yamanaka, Tatsuya Nakaoka, Katsutoshi Takaki, Daiki Fukushima, Naoto Kojiguchi, Kazunari Masumoto, Katsura Matsumoto, Hiroshi Akitaya, Ryosuke Itoh, Yuka Kanda, Yuki Moritani, Koji Takata, Makoto Uemura, Takahiro Ui, Michitoshi Yoshida, Takashi Hattori, Chien-Hsiu Lee, Nozomu Tominaga, Ken’ichi Nomoto |
| 概要 | <jats:title>Abstract</jats:title>
<jats:p>We present optical and near-infrared observations of the nearby Type Iax supernova (SN) 2014dt from 14 to 410 d after the maximum light. The velocities of the iron absorption lines in the early phase indicated that SN 2014dt showed slower expansion than the well-observed Type Iax SNe 2002cx, 2005hk, and 2012Z. In the late phase, the evolution of the light curve and that of the spectra were considerably slower. The spectral energy distribution kept roughly the same shape after ∼100 d, and the bolometric light curve flattened during the same period. These observations suggest the existence of an optically thick component that almost fully trapped the γ-ray energy from 56Co decay. These findings are consistent with the predictions of the weak deflagration model, leaving a bound white dwarf remnant after the explosion.</jats:p> |
| DOI | 10.1093/pasj/psy116 |
| ISSN | 00046264 |
| NAID | 1360004234736478848 |