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| Paper: |
Helium Stars as Supernova Progenitor |
| Volume: |
391, Hydrogen-Deficient Stars |
| Page: |
359 |
| Authors: |
Waldman, R.; Yungelson, L.R.; Barkat, Z. |
| Abstract: |
We follow the evolution of helium stars of initial mass (2.2 − 2.5)M⊙, and show that they undergo off-center carbon burning, which leaves behind ∼0.01M⊙ of unburnt carbon in the inner part of the core. When the carbon-oxygen core grows to Chandrasekhar mass, the amount of left-over carbon is sufficient to ignite thermonuclear runaway. At the moment of explosion, the star will possess an envelope of several 0.1M⊙, consisting of He, C, and possibly some H, perhaps producing a kind of peculiar SN. Based on the results of Waldman & Barkat (2007) for accreting white dwarfs, we expect to get thermonuclear runaway at a broad range of ρc ≈ (1 − 6) × 109g cm−3, depending on the amount of residual carbon. We verified the feasibility of this scenario by showing that in a close binary system with initial masses (8.5+7.7)M⊙ and initial period of 150 day the primary produces a helium remnant of 2.3M⊙ that evolves further like the model we considered. |
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