Helium stars as supernova progenitors
| dc.creator | Waldman, Roni | |
| dc.creator | Yungelson, Lev R. | |
| dc.creator | Barkat, Zalman | |
| dc.date | 2007-10-21 | |
| dc.date.accessioned | 2026-07-07T08:37:38Z | |
| dc.date.available | 2026-07-07T08:37:38Z | |
| dc.description | We follow the evolution of helium stars of initial mass $(2.2 - 2.5) M_\odot$, and show that they undergo off-center carbon burning, which leaves behind ${\mathbf \sim 0.01 M_\odot}$ 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 $0.1 M_{\odot}$, consisting of He, C, and possibly some H, perhaps producing a kind of peculiar SN. Based on the results of Waldman and Barkat (2007) for accreting white dwarfs, we expect to get thermonuclear runaway at a broad range of $ρ_c \approx (1 - 6) \times 10^9 \mathrm{g cm^{-3}}$, 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 $(8.5 + 7.7) M_{\odot}$ and initial period of 150 day the primary produces a helium remnant of $2.3 M_{\odot}$ that evolves further like the model we considered. | |
| dc.description | 4 pages, 2 figures, to appear in Hydrogen-Deficient Stars 2007 | |
| dc.identifier | https://arxiv.org/abs/0710.3911 | |
| dc.identifier | http://arxiv.org/abs/0710.3911 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/140468 | |
| dc.subject | Astrophysics | |
| dc.title | Helium stars as supernova progenitors | |
| dc.type | text |