2020/03/04 by L. Xue, Li Xue, Cheng-Liang Jiao +1
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Gamma-ray bursts and supernovae #Magnetic field #Physics #Polar #Stars #Stellar, planetary, and galactic studies #Supernova #Supernova remnant #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1093/mnras/staa3696
9 pages, 13 figures, submitted to MNRAS
arxiv created 2020/03/04 · openalex publication_date 2020/11/26 · arxiv updated 2020/12/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT We run 3D numerical simulations for the accretion flow around the white dwarf (WD) in the progenitor system of Tycho’s supernova (SN). The mass of the WD, mass of the companion star, and the orbital period are set to be 1M⊙, 1.6M⊙, and 0.794 d, respectively, based on theoretical and observational researches of Tycho’s SN remnant (SNR). We find that when the magnetic field in the accreted material is negligible, outflowing wind is concentrated near the equatorial plane. When the magnetic field has energy equipartition with internal energy, polar wind is comparable with the equatorial wind. A carefully chosen magnetic field between the above two cases (B=5.44× 103 \rm G) can roughly reproduce the latitude-dependent wind required to form the peculiar periphery of Tycho’s SNR. Including a reasonable amount of viscosity in the calculation does not change our conclusion.