Supernova Explosions and Neutron Star Formation
Supernova Explosions and Neutron Star Formation
复制标题
超新星爆炸和中子星形成
DOI：
10.1007/3-540-44578-1_13
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发表时间：
2001
期刊：
影响因子：
--
通讯作者：
M. Rampp
中科院分区：
文献类型：
--
作者：
H. Janka;K. Kifonidis;M. Rampp
综述了大质量恒星坍缩、爆炸和中子星形成的现状。然而，根据人们喜欢的设想，中微子存款在围绕新生中子星星的恒星介质中储存爆炸的能量，这一点并没有得到证实和无可争议。特别是对超新星1987 A的观测表明，混合过程在膨胀的星星中起着重要作用，多维模拟表明，这些过程与中子星星附近的对流不稳定性有关。中子星星内部对流增强的能量传输对中微子发射和中微子加热机制有重要影响。这也适用于在核密度下中微子相互作用的抑制。多维流体力学、广义相对论和更好地理解中子星星物质中的中微子相互作用，对于解决最先进的球形模型即使通过求解玻尔兹曼方程非常精确地处理中微子输运也不会产生爆炸的问题可能至关重要。
The current picture of the collapse and explosion of massive stars and the formation of neutron stars is reviewed. According to the favored scenario, however by no means proven and undisputed, neutrinos deposit the energy of the explosion in the stellar medium which surrounds the nascent neutron star. Observations, in particular of Supernova 1987A, suggest that mixing processes play an important role in the expanding star, and multi-dimensional simulations show that these are linked to convective instabilities in the immediate vicinity of the neutron star. Convectively enhanced energy transport inside the neutron star can have important consequences for the neutrino emission and thus the neutrino-heating mechanism. This also holds for a suppression of the neutrino interactions at nuclear densities. Multi-dimensional hydrodynamics, general relativity, and a better understanding of the neutrino interactions in neutron star matter may be crucial to resolve the problem that state-of-the-art spherical models not yield explosions even with a very accurate treatment of neutrino transport by solving the Boltzmann equation.