Helium star donors to thermonuclear supernovae
Description
We perform binary evolution calculations of helium star - carbon-oxygen white dwarf binaries using the stellar evolution code MESA. We focus on 1-2 Msun He stars that undergo thermal-timescale mass transfer. We survey the initial binary parameters (orbital period and He star mass) and determine which systems can evolve towards thermonuclear supernovae. Our time-dependent calculations resolve the stellar structures of both binary components, which allows accurate detection of the occurrence of off-center carbon ignitions. We find systems that successfully reach explosion generally have orbital periods of hours; it will be useful to understand the MW population of He star - WD binaries with these properties. We also describe the observational appearance of these systems near the time of explosion as they may be detectable in pre-explosion images of supernovae.
Files
Wong_Schwab_sdOB9_ad.pdf
Files
(5.8 MB)
Name | Size | Download all |
---|---|---|
md5:7f32a172b7ebc972e069542172399ed9
|
4.6 MB | Preview Download |
md5:7204c07101126cc632b4ac4b66844baf
|
1.2 MB | Preview Download |