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The dynamics of neutrino-driven supernova explosions after shock revival in 2D and 3D

机译:2D和3D激振后中微子驱动的超新星爆炸的动力学

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摘要

We study the growth of the explosion energy after shock revival in neutrino-driven explosions in two and three dimensions (2D/3D) using multi-group neutrino hydrodynamics simulations of an 11.2 M⊙ star. The 3D model shows a faster and steadier growth of the explosion energy and already shows signs of subsiding accretion after one second. By contrast, the growth of the explosion energy in 2D is unsteady, and accretion lasts for several seconds as confirmed by additional long-time simulations of stars of similar masses. Appreciable explosion energies can still be reached, albeit at the expense of rather high neutron star masses. In 2D, the binding energy at the gain radius is larger because the strong excitation of downward-propagating g modes removes energy from the freshly accreted material in the downflows. Consequently, the mass outflow rate is considerably lower in 2D than in 3D. This is only partially compensated by additional heating by outward-propagating acoustic waves in 2D. Moreover, the mass outflow rate in 2D is reduced because much of the neutrino energy deposition occurs in downflows or bubbles confined by secondary shocks without driving outflows. Episodic constriction of outflows and vertical mixing of colder shocked material and hot, neutrino-heated ejecta due to Rayleigh–Taylor instability further hamper the growth of the explosion energy in 2D. Further simulations will be necessary to determine whether these effects are generic over a wider range of supernova progenitors.
机译:我们使用11.2M⊙星的多组中微子流体动力学模拟研究了中微子驱动的爆炸在二维和二维(2D / 3D)中激振后爆炸能量的增长。 3D模型显示爆炸能量更快,更稳定地增长,并且在一秒钟后已经显示出沉降的迹象。相反,爆炸能量在2D中的增长不稳定,并且积聚持续几秒钟,这一点已通过对相似质量的恒星进行的其他长时间模拟得到证实。尽管以相当高的中子星质量为代价,仍然可以达到可观的爆炸能量。在2D中,增益半径处的结合能更大,这是因为向下传播的g模式的强烈激发将能量从下行流中的新堆积材料中移除。因此,质量流出率在2D中明显低于3D。这只能通过2D向外传播的声波的额外加热来部分补偿。而且,由于中微子能量的大部分沉积发生在由二次冲击限制的下流或气泡中,而没有驱动外流,因此二维中的质量外流率降低了。由于瑞利-泰勒(Rayleigh-Taylor)的不稳定性,流出的收缩和较冷的冲击材料以及中微子加热的热喷射流的垂直混合进一步阻碍了2D爆炸能量的增长。为了确定这些影响是否在更广泛的超新星祖细胞中普遍存在,将需要进行进一步的模拟。

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    Muller B.;

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  • 年度 2015
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  • 原文格式 PDF
  • 正文语种 eng
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