Abstract
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.
| Original language | English |
|---|---|
| Pages (from-to) | L23-L27 |
| Journal | Astrophysical Journal |
| Volume | 361 |
| Issue number | 1 PART 2 |
| DOIs | |
| Publication status | Published - Sep 20 1990 |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Low-mass helium star models for type Ib supernovae : Light curves, mixing, and nucleosynthesis. / Shigeyama, Toshikazu; Nomoto, Ken'ichi; Tsujimoto, Takuji; Hashimoto, Masa Aki.
In: Astrophysical Journal, Vol. 361, No. 1 PART 2, 20.09.1990, p. L23-L27.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Low-mass helium star models for type Ib supernovae
T2 - Light curves, mixing, and nucleosynthesis
AU - Shigeyama, Toshikazu
AU - Nomoto, Ken'ichi
AU - Tsujimoto, Takuji
AU - Hashimoto, Masa Aki
PY - 1990/9/20
Y1 - 1990/9/20
N2 - 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.
AB - 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.
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U2 - 10.1086/185818
DO - 10.1086/185818
M3 - Article
AN - SCOPUS:0002498339
VL - 361
SP - L23-L27
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 PART 2
ER -