2016/03/01 by P. Neunteufel, S. -C. Yoon, S.-C. Yoon +1 · 2 citations
Physics and Astronomy · #Accretion (finance) #Astronomy and Astrophysical Research #Chandrasekhar limit #Gamma-ray bursts and supernovae #Scientific Research and Discoveries #Stellar evolution #Supernova #Thermonuclear fusion #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201527845
published as A&A 589, A43 (2016) · 12 pages, 11 figures. To be published in A&A, accepted 04/02/2016
openalex publication_date 2016/03/01 · arxiv created 2016/03/02 · arxiv updated 2016/04/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. Type Ia supernovae (SNe Ia) have been an important tool for astronomy for quite some time; however, the nature of their progenitors remains somewhat mysterious. Recent theoretical studies indicated the possibility of producing thermonuclear detonations of carbon-oxygen white dwarfs (CO WDs) at masses less than the Chandrasekhar mass through accretion of helium-rich matter, which would, depending on mass accretion rate, mass, and initial temperature of the WD, spectrally resemble either a normal SN Ia or a peculiar one.