Low-mass helium star models for type Ib supernovae: Light curves, mixing, and nucleosynthesis

Toshikazu Shigeyama, Ken'ichi Nomoto, Takuji Tsujimoto, Masa Aki Hashimoto

研究成果: Contribution to journalArticle査読

84 被引用数 (Scopus)

抄録

Light curves, Rayleigh-Taylor instability, and nucleosynthesis of exploding helium stars are examined to look for relevant models for Type Ib supernovae, especially for SN 1983N and 19831 whose light curves decline as fast as Type Ia supernovae. The calculated light curves show a systematic dependence on the stellar mass, because smaller mass helium stars undergo more extensive mixing and eject smaller mass, thereby forming light curves with steeper tails. The relatively fast decline of the SN Ib light curves can thus be accounted for by the helium star models if the helium star mass is as low as 3-4 M and if 56Ni is mixed to the surface layers. Moreover, the 3-4 M helium stars, having relatively small mass iron cores, can produce ∼0.15 M 56Ni as required from the maximum luminosities. In terms of nucleosynthesis, mixing, and light curves, the helium stars of 3-4 M (which form from stars with Mms ∼ 12-16 M in binary systems) are the most relevant progenitors of the Type Ib supernovae 1983N and 19831.

本文言語英語
ページ(範囲)L23-L27
ジャーナルAstrophysical Journal
361
1 PART 2
DOI
出版ステータス出版済み - 9 20 1990

All Science Journal Classification (ASJC) codes

  • 天文学と天体物理学
  • 宇宙惑星科学

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