Query : 2010A&A...523A...3L

2010A&A...523A...3L - Astronomy and Astrophysics, volume 523, A3-3 (2010/11-2)

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae.

LIU W.-M., CHEN W.-C., WANG B. and HAN Z.W.

Abstract (from CDS):

The recent discovery of several overluminous type Ia supernovae (SNe Ia) indicates that the explosive masses of white dwarfs may significantly exceed the canonical Chandrasekhar-mass limit. Rapid differential rotation may support these massive white dwarfs (WDs). Based on the single-degenerate scenario and assuming that the WDs would differentially rotate when the accretion rate {dot}(M)>3x10–7M/yr, we performed the numerical calculations for ∼1000 binary systems consisting of a He star and a CO WD with Eggleton's stellar evolution code. We present the initial parameters in the orbital period - helium star-mass plane (for WD masses of 1.0M and 1.2M, respectively), which lead to super-Chandrasekhar mass SNe Ia. Our results indicate that for an initially massive WD of 1.2M, a large number of SNe Ia may result from super-Chandrasekhar mass WDs. The highest mass of the WD at the moment of the SNe Ia explosion is 1.81M, but very massive (>1.85M) WDs cannot be formed. However, when the initial mass of WDs is 1.0M, the explosive masses of SNe Ia are nearly uniform, which is consistent with the rareness of super-Chandrasekhar mass SNe Ia in observations.

Abstract Copyright:

Journal keyword(s): binaries: general - stars: rotation - stars: evolution - supernovae: general - white dwarfs

Simbad objects: 2

goto Full paper

goto View the references in ADS

Number of rows : 2
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 HD 49798 HXB 06 48 04.7001531360 -44 18 58.436036028 6.758 8.017 8.287 8.391 8.543 sdO6 319 0
2 V* V445 Pup No* 07 37 56.8797787992 -25 56 58.837610328       13.654 12.849 ~ 170 0

To bookmark this query, right click on this link: simbad:objects in 2010A&A...523A...3L and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact