2012/07/18 by Wolfgang E. Kerzendorf, Wolfgang Kerzendorf, B. Schmidt +5 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Chandrasekhar limit #Gamma-ray bursts and supernovae #Nuclear physics #Physics #Plasma #Stars #Stellar, planetary, and galactic studies #Supernova #Thermonuclear fusion #White dwarf #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/759/1/7
11 pages, accepted by ApJ
arxiv created 2012/07/18 · openalex publication_date 2012/10/11 · arxiv updated 2015/06/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Type Ia supernovae play a significant role in the evolution of the universe and have a wide range of applications. It is widely believed that these events are the thermonuclear explosions of carbon–oxygen white dwarfs close to the Chandrasekhar mass (1.38 M ☉ ). However, CO white dwarfs are born with masses much below the Chandrasekhar limit and thus require mass accretion to become Type Ia supernovae. There are two main scenarios for accretion: first, the merger of two white dwarfs and, second, a stable mass accretion from a companion star. According to predictions, this companion star (also referred to as donor star) survives the explosion and thus should be visible in the center of Type Ia remnants. In this paper, we scrutinize the central stars (79 in total) of the SN 1006 remnant to search for the surviving donor star as predicted by this scenario. We find no star consistent with the traditional accretion scenario in SN 1006.