2004/02/12 by Sung-Chul Yoon, S. -C. Yoon, N. Langer · 3 citations
Physics and Astronomy · #Accretion (finance) #Angular momentum #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Atomic physics #Chandrasekhar limit #Gamma-ray bursts and supernovae #Helium #Physics #Stars #Stellar evolution #Stellar, planetary, and galactic studies #Supernova #White dwarf #astro-ph
paper · pdf · doi:10.1051/0004-6361:20035823
published as Astron.Astrophys. 419 (2004) 645 · 8 pages, 5 figures, Accepted to A&A
arxiv created 2004/02/12 · openalex publication_date 2004/05/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present evolutionary models of helium-accreting carbon-oxygen white dwarfs in which we include the effects of the spin-up of the accreting star induced by angular momentum accretion, rotationally induced chemical mixing and rotational energy dissipation. Initial masses of 0.6 and 0.8 and constant accretion rates of a few times of helium-rich matter have been considered, which is typical for the sub-Chandrasekhar mass progenitor scenario for Type Ia supernovae. It is found that the helium envelope in an accreting white dwarf is heated efficiently by friction in the differentially rotating spun-up layers. As a result, helium ignites much earlier and under much less degenerate conditions compared to the corresponding non-rotating case. Consequently, a helium detonation may be avoided, which questions the sub-Chandrasekhar mass progenitor scenario for Type Ia supernovae. We discuss implications of our results for the evolution of helium star plus white dwarf binary systems as possible progenitors of recurrent helium novae.