2019/01/20 by Iminhaji Ablimit, Keiichi Maeda · 20 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Binary number #Gamma-ray bursts and supernovae #Magnetic field #Physics #Polar #Roche lobe #Stars #Stellar, planetary, and galactic studies #Supernova #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/aaf722
published in The Astrophysical Journal 871(1), 31 (IOP Publishing) · Published in ApJ
openalex publication_date 2019/01/20 · arxiv created 2019/06/06 · arxiv updated 2019/06/07 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract With the increasing number of observed magnetic white dwarfs (WDs), the role of the magnetic field of the WD in both single and binary evolutions should attract more attention. In this study, we investigate the WD/main-sequence star binary evolution with the Modules for Experiments in Stellar Astrophysics code, by considering WDs with non-, intermediate, and high magnetic field strength. We mainly focus on how the strong magnetic field of the WD (in a polar-like system) affects the binary evolution toward Type Ia supernovae (SNe Ia). The accreted matter goes along the magnetic field lines and falls down onto polar caps, and it can be confined by the strong magnetic field of the WD, so that the enhanced isotropic pole-mass transfer rate can let the WD grow in mass even with a low mass donor with a low Roche-lobe overflow mass transfer rate. The results from the magnetic confinement model show that both the initial parameter space for SNe Ia and characteristics of the donors after SNe Ia are easily distinguishable from those found in previous SNe Ia progenitor models. The predicted natures of the donors are compatible with the non-detection of a companion in several SN remnants and nearby SNe.