Abstract
Taking into account the rotation of mass-accreting white dwarfs (WDs) whose masses exceed the Chandrasekhar mass, we extend our new single degenerate model for the progenitors of Type Ia supernovae (SNe Ia), accounting for two types of binary systems: those with a main-sequence companion and those with a red-giant (RG) companion. We present a mass distribution of WDs exploding as SNe Ia, where the WD mass ranges from 1.38 to 2.3 M ⊙. These progenitor models are assigned to various types of SNe Ia. A lower mass range of WDs (1.38 M ⊙ < M WD ≲ 1.5 M ⊙), which are supported by rigid rotation, corresponds to normal SNe Ia. A variety of spin-down time may lead to a variation of brightness. A higher mass range of WDs (M WD ≳ 1.5 M ⊙), which are supported by differential rotation, corresponds to brighter SNe Ia such as SN 1991T. In this case, a variety of the WD mass may lead to a variation of brightness. We also show the evolutionary states of the companion stars at SN Ia explosions and pose constraints on the unseen companions. In the WD+RG systems, in particular, most of the RG companions have evolved to helium/carbon-oxygen WDs in the spin-down phase before the SN Ia explosions. In such a case, we do not expect any prominent signature of the companion immediately before and after the explosion. We also compare our new models with the recent stringent constraints on the unseen progenitors of SNe Ia such as SN 2011fe.
| Original language | English |
|---|---|
| Article number | L4 |
| Journal | Astrophysical Journal Letters |
| Volume | 756 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 2012 |
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Keywords
- binaries: close
- stars: winds, outflows
- supernovae: general
- supernovae: individual (SN 2011fe)
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
Final fates of rotating white dwarfs and their companions in the single degenerate model of type Ia supernovae. / Hachisu, Izumi; Kato, Mariko; Nomoto, Ken'Ichi.
In: Astrophysical Journal Letters, Vol. 756, No. 1, L4, 2012.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Final fates of rotating white dwarfs and their companions in the single degenerate model of type Ia supernovae
AU - Hachisu, Izumi
AU - Kato, Mariko
AU - Nomoto, Ken'Ichi
PY - 2012
Y1 - 2012
N2 - Taking into account the rotation of mass-accreting white dwarfs (WDs) whose masses exceed the Chandrasekhar mass, we extend our new single degenerate model for the progenitors of Type Ia supernovae (SNe Ia), accounting for two types of binary systems: those with a main-sequence companion and those with a red-giant (RG) companion. We present a mass distribution of WDs exploding as SNe Ia, where the WD mass ranges from 1.38 to 2.3 M ⊙. These progenitor models are assigned to various types of SNe Ia. A lower mass range of WDs (1.38 M ⊙ < M WD ≲ 1.5 M ⊙), which are supported by rigid rotation, corresponds to normal SNe Ia. A variety of spin-down time may lead to a variation of brightness. A higher mass range of WDs (M WD ≳ 1.5 M ⊙), which are supported by differential rotation, corresponds to brighter SNe Ia such as SN 1991T. In this case, a variety of the WD mass may lead to a variation of brightness. We also show the evolutionary states of the companion stars at SN Ia explosions and pose constraints on the unseen companions. In the WD+RG systems, in particular, most of the RG companions have evolved to helium/carbon-oxygen WDs in the spin-down phase before the SN Ia explosions. In such a case, we do not expect any prominent signature of the companion immediately before and after the explosion. We also compare our new models with the recent stringent constraints on the unseen progenitors of SNe Ia such as SN 2011fe.
AB - Taking into account the rotation of mass-accreting white dwarfs (WDs) whose masses exceed the Chandrasekhar mass, we extend our new single degenerate model for the progenitors of Type Ia supernovae (SNe Ia), accounting for two types of binary systems: those with a main-sequence companion and those with a red-giant (RG) companion. We present a mass distribution of WDs exploding as SNe Ia, where the WD mass ranges from 1.38 to 2.3 M ⊙. These progenitor models are assigned to various types of SNe Ia. A lower mass range of WDs (1.38 M ⊙ < M WD ≲ 1.5 M ⊙), which are supported by rigid rotation, corresponds to normal SNe Ia. A variety of spin-down time may lead to a variation of brightness. A higher mass range of WDs (M WD ≳ 1.5 M ⊙), which are supported by differential rotation, corresponds to brighter SNe Ia such as SN 1991T. In this case, a variety of the WD mass may lead to a variation of brightness. We also show the evolutionary states of the companion stars at SN Ia explosions and pose constraints on the unseen companions. In the WD+RG systems, in particular, most of the RG companions have evolved to helium/carbon-oxygen WDs in the spin-down phase before the SN Ia explosions. In such a case, we do not expect any prominent signature of the companion immediately before and after the explosion. We also compare our new models with the recent stringent constraints on the unseen progenitors of SNe Ia such as SN 2011fe.
KW - binaries: close
KW - stars: winds, outflows
KW - supernovae: general
KW - supernovae: individual (SN 2011fe)
UR - http://www.scopus.com/inward/record.url?scp=84865186997&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84865186997&partnerID=8YFLogxK
U2 - 10.1088/2041-8205/756/1/L4
DO - 10.1088/2041-8205/756/1/L4
M3 - Article
AN - SCOPUS:84865186997
VL - 756
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1
M1 - L4
ER -