Three dimensional numerical simulation of mixing in supernova explosions

超新星爆炸混合的三维数值模拟

基本信息

批准号：
04640272
负责人：
HACHISU Izumi
金额：
$ 1.41万
依托单位：
University of Tokyo
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (C)
财政年份：
1992
资助国家：
日本
起止时间：
1992 至 1993
项目状态：
已结题

项目摘要

We calculate a nonlinear growth of the Rayleigh-Taylor instability in the exploding red supergiant stars with a two-dimensional hydrodynamical code, and examine how the extent of mixing depends of the progenitor's core mass and the envelope mass. The results are compared with the observations of type II-P supernovae and the recent type II-b supernova 1993J.It has been suggested that the duration of the plateau of Type II-P supernova light curves depends on the extent of inward mixing of hydrogen in the supernova ejecta. We have followed numerically a nonlinear growth of the Rayleigh-Taylor (R-T) instability in the exploding red super-giant stars with a two-dimensional (2-D) hydro-dynamical code, and examined whether or not the R-T mixing is large enough to account for the plateau length of Type II-P supernova light curves. The inward mixing of hydrogen into the core at expansion velocities of 500-800kms^<-1> is confirmed for the two red-supergiant models with the main-sequence masses o … More f 13 M_<<of sun>> and 20 M_<<of sun>>. Mixing of hydrogen is extensive enough to reproduce the plateau of light curves even with a very small amplitude of the initial perturbations such as - 0.2%. However, the outward mixing of ^<56>Ni is so defferent between the two progenitors. The nickel is mixed up to the middle of the hydrogen-rich envelope in the 13 M_<<of sun>>, while it is hardly mixed for the 20 M_<<of sun>> stars. These differences in the mixing may affect the shape of light curves.It has been suggested that the duration of the plateau of Type II-P supernova light curves depends on the extent of inward mixing of hydrogen in the supernova ejecta. We have followed numerically a nonlinear growth of the Rayleigh-Taylor (R-T) instability in the exploding red super-giant stars with a two-dimensional (2-D) hydro-dynamical code, and examined whether or not the R-T mixing is large enough to account for the plateau length of Type II-P supernova light curves. The inward mixing of hydrogen into the core at expansion velocities of 500-800kms^<-1> is confirmed for the two red-supergiant models with the main-sequence masses of 13 M_<<of sun>> and 20 M_<<of sun>>. Mixing of hydrogen is extensive enough to reproduce the plateau of light curves even with a very small amplitude of the initial perturbations such as - 0.2%. However, the outward mixing of ^<56>Ni is so defferent between the two progenitors. The nickel is mixed up to the middle of the hydrogen-rich envelope in the 13 M_<<of sun>>, while it is hardly mixed for the 20 M_<<of sun>> stars. These differences in the mixing may affect the shape of light curves. Less

我们用二维水力学代码计算雷利 - 泰勒不稳定性的非线性生长，并检查混合程度如何取决于祖细胞的核心质量和包膜质量。将结果与II-P型超新星的观察结果和最近的II-B型超新星1993J进行了比较。已提出，II-P型Supernova型光曲线的高原持续时间取决于氢In supernova ejecta的内向混合的程度。我们遵循了带有二维（2-D）流体动力学的爆炸红色超级巨星中雷利 - 泰勒（R-T）不稳定性的众多非线性生长，并检查了R-T混合是否足以说明II II型II-P Supernova轻曲线的高原长度。确认了两个红色苏植物模型的膨胀速度以500-800kms^<-1>的膨胀速度混合到核心中。即使使用很小的初始扰动的放大器，例如-0.2％，氢的混合也足够广泛，可以重现光曲线的高原。但是， ^<56> ni的外部混合在两个祖细胞之间如此较低。在13 m _ <<的太阳>>中，将镍混合到富含氢的信封的中间，而对于20 m _ <<的太阳>>恒星几乎没有混合。混合中的这些差异可能会影响光曲线的形状。已经提出，II-P型超新星光曲线的高原持续时间取决于超新星喷射中氢的内向混合的程度。我们遵循了雷利 - 泰勒（R-T）不稳定性在爆炸的红色超级巨星中的非线性生长，其具有二维（2-D）水力学代码，并检查了R-T混合是否足以说明II型II-P Supernova轻曲线的高原长度。对于两个红色苏植物模型的膨胀速度，氢的内向混合在500-800kms^<-1>的膨胀速度下，具有13 m _ <<的主要序列质量，Sun >>和20 m _ <<的Sun >>。即使使用很小的初始扰动的放大器，例如-0.2％，氢的混合也足够广泛，可以重现光曲线的高原。但是， ^<56> ni的外部混合在两个祖细胞之间如此较低。在13 m _ <<的太阳>>中，将镍混合到富含氢的信封的中间，而对于20 m _ <<的太阳>>恒星几乎没有混合。混合中的这些差异可能会影响光曲线的形状。较少的