A COMPREHENSIVE PROGENITOR MODEL FOR SNe Ia

作者：Meng, X.^*; Yang, W.

来源：Astrophysical Journal, 2010, 710(2): 1310-1323.

DOI：10.1088/0004-637X/710/2/1310

• binaries: close
• stars: evolution
• stars: dwarf novae
• supernovae: general
• white dwarfs

Although the nature of the progenitor of Type Ia supernovae (SNe Ia) is still unclear, the single-degenerate (SD) channel for the progenitor is currently accepted, in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from its companion, increases its mass to the Chandrasekhar mass limit, and then explodes as an SN Ia. The companion may be a main sequence or a slightly evolved star (WD + MS), or a red giant star (WD + RG). Incorporating the effect of mass stripping and accretion-disk instability on the evolution of the WD binary, we carried out binary stellar evolution calculations for more than 1600 close WD binaries. As a result, the initial parameter spaces for SNe Ia are presented in an orbital period-secondary mass (log P-i, M-2(i)) plane. We confirmed that in a WD + MS system, the initial companion leading to SNe Ia may have mass from 1 M-circle dot to 5 M-circle dot. The initial WD mass for SNe Ia from WD + MS channel is as low as 0.565 M-circle dot, while the lowest WD mass from the WD + RG channel is 1.0 M-circle dot. Adopting the above results, we studied the birth rate of SNe Ia via a binary population synthesis approach. We found that the Galactic SNe Ia birth rate from SD model is (2.55-2.9) x 10(-3) yr(-1) (including WD + He star channel), which is slightly smaller than that from observation. If a single starburst is assumed, the distribution of the delay time of SNe Ia from the SD model may be a weak bimodality, where WD + He channel contributes to SNe Ia with delay time shorter than 10(8) yr and WD + RG channel to those with age longer than 6 Gyr.

• 出版日期2010-2-20
• 单位河南理工大学