论文标题
Tycho超新星祖细胞中积聚流的三维模拟
Three-dimensional simulations of accretion flow in the progenitor of Tycho's supernova
论文作者
论文摘要
我们在Tycho的Supernova（SN）的祖细胞系统中运行了三维数值模拟，以围绕白色矮人（WD）的积聚流。根据Tycho的SN Remnant（SNR）的理论和观察性研究，分别分别基于理论和观察性研究（SNR）的理论和观察性研究。我们发现，当积聚材料中的磁场可忽略不计时，偏远的风被集中在赤道平面附近。当磁场带有内部能量的能量等级时，极风与赤道风相当。在上述两种情况之间进行了精心选择的磁场（$ b = 5.44 \ times10^3 \ rm {g} $）可以粗略地重现形成Tycho snr的特殊外围所需的纬度依赖风。
We run three-dimensional numerical simulations for the accretion flow around the white dwarf (WD) in the progenitor system of Tycho's supernova (SN). The mass of the WD, mass of the companion star, and the orbital period are set to be 1$M_{\odot}$, 1.6$M_{\odot}$, and 0.794 day, respectively, based on theoretical and observational researches of Tycho's SN remnant (SNR). We find that when the magnetic field in the accreted material is negligible, outflowing wind is concentrated near the equatorial plane. When the magnetic field has energy equipartition with internal energy, polar wind is comparable with the equatorial wind. A carefully chosen magnetic field between the above two cases ($B=5.44\times10^3 \rm{G}$) can roughly reproduce the latitude-dependent wind required to form the peculiar periphery of Tycho's SNR.
