2018/02/28 by Xiangcun Meng, Xiang-Cun Meng, Zhanwen Han +1 · 5 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Neutrino Physics Research #Phase (matter) #Signature (topology) #Supernova #Type (biology) #White dwarf #astro-ph.HE
paper · pdf · doi:10.3847/2041-8213/aab159
published in The Astrophysical Journal Letters 855(2), L18 (IOP Publishing) · 2 figures, ApJ Letter on line
openalex created_date 2018/03/06 · openalex publication_date 2018/03/07 · arxiv created 2018/03/08 · arxiv updated 2018/03/21 · openalex updated_date 2026/08/05
Abstract Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact progenitor nature is still unclear. A basic method to distinguish the different progenitor models is to search the signal from the single-degenerate (SD) model, e.g., the signal for the existence of a nondegenerate companion before or after supernova explosion. Observationally, some SNe Ia show such signals, while the others do not. Here, we propose a universal model to explain these observations based on the spin-up/spin-down model, in which a white dwarf (WD) will experience a spin-down phase before supernova explosion, and the spin-down timescale is determined by its initial mass, i.e., the more massive the initial WD, the shorter the spin-down timescale and then the more likely the SN Ia is to show the SD signature. Therefore, our model predicts that the SNe Ia from hybrid carbon–oxygen–neon WDs are more likely to show the SD signature observationally, as some peculiar SNe Ia showed.