The Type I[CLC]c[/CLC] Hypernova SN 2002[CLC]ap[/CLC]
| Autor: | Takeo Minezaki, J. Deng, George Kosugi, Stefano Benetti, Koichi Iwamoto, Massimo Turatto, Keigo Enya, Kenzo Kinugasa, Stephen J. Smartt, Yuzuru Yoshii, Hiroyuki Tomita, Ryan Chornock, Kazuya Ayani, Gang Zhao, Keiichi Maeda, Hideyo Kawakita, Nobunari Kashikawa, Alexei V. Filippenko, Masanori Iye, Kentaro Motohara, Ken'ichi Nomoto, Kazuhito Hatano, Y. Ohyama, Hitoshi Yamaoka, Yukiyasu Kobayashi, Mamoru Doi, Robert A. Fesen, Koji S. Kawabata, T. Kawabata, H. Umeda, Paolo A. Mazzali, Yulei Qiu, Christopher L. Gerardy, Masahide Takada-Hidai |
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| Rok vydání: | 2002 |
| Předmět: | |
| Zdroj: | The Astrophysical Journal. 572:L61-L65 |
| ISSN: | 1538-4357 0004-637X |
| DOI: | 10.1086/341504 |
| Popis: | Photometric and spectroscopic data of the energetic Type Ic supernova (SN) 2002ap are presented, and the properties of the SN are investigated through models of its spectral evolution and its light curve. The SN is spectroscopically similar to the hypernova SN 1997ef. However, its kinetic energy [~(4-10) ? 1051 ergs] and the mass ejected (2.5-5 M?) are smaller, resulting in a faster evolving light curve. The SN synthesized ~0.07 M? of 56Ni, and its peak luminosity was similar to that of normal SNe. Brightness alone should not be used to define a hypernova, whose defining character, namely very broad spectral features, is the result of high kinetic energy. The likely main-sequence mass of the progenitor star was 20-25 M?, which is also lower than that of both hypernovae SN 1997ef and SN 1998bw. SN 2002ap appears to lie at the low-energy and low-mass end of the hypernova sequence as it is known so far. Observations of the nebular spectrum, which is expected to dominate by the summer of 2002, are necessary to confirm these values. |
| Databáze: | OpenAIRE |
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