2003A&A...412L..53Y


Query : 2003A&A...412L..53Y

2003A&A...412L..53Y - Astronomy and Astrophysics, volume 412, L53-56 (2003/12-3)

The first binary star evolution model producing a Chandrasekhar mass white dwarf.

YOON S.-C. and LANGER N.

Abstract (from CDS):

Today, Type Ia supernovae are essential tools for cosmology, and recognized as major contributors to the chemical evolution of galaxies. The construction of detailed supernova progenitor models, however, was so far prevented by various physical and numerical difficulties in simulating binary systems with an accreting white dwarf component, e.g., unstable helium shell burning which may cause significant expansion and mass loss. Here, we present the first binary evolution calculation which models both stellar components and the binary interaction simultaneously, and where the white dwarf mass grows up to the Chandrasekhar limit by mass accretion. Our model starts with a 1.6M helium star and a 1.0M CO white dwarf in a 0.124-day orbit. Thermally unstable mass transfer starts when the CO core of the helium star reaches 0.53M, with mass transfer rates of 1...8x10–6M/yr. The white dwarf burns the accreted helium steadily until the white dwarf mass has reached ∼1.3M and weak thermal pulses follow until carbon ignites in the center when the white dwarf reaches 1.37M. Although the supernova production rate through this channel is not well known, and this channel can not be the only one as its progenitor life time is rather short (∼107-108yr), our results indicate that helium star plus white dwarf systems form a reliable route for producing Type Ia supernovae.

Abstract Copyright:

Journal keyword(s): stars: evolution - stars: white dwarf - stars: helium - stars: binary - stars: supernova - supernovae: Type Ia

Simbad objects: 2

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Number of rows : 2
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 2E 0035.4-7229 XB* 00 37 19.6683991960 -72 14 13.187852739   20.0 20.2     ~ 102 0
2 RX J0537.6-7033 XB* 05 37 43.0 -70 34 15           ~ 31 0

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