Strangeness condensation and cooling of neutron stars.
Strangeness condensation and cooling of neutron stars.
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DOI：
10.1103/physrevd.37.2042
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发表时间：
1988-04
期刊：
影响因子：
--
通讯作者：
Brown;Kubodera;Page;Pizzochero
中科院分区：
文献类型：
--
作者：
Brown;Kubodera;Page;Pizzochero
本文计算了密度为2.3- 3.0倍核物质密度的致密中子物质中奇异凝聚的可能效应，并特别参考了可能形成于SN 1987 A的中子星星的冷却。虽然中子星星的中心在奇异凝聚的存在下会比通过传统机制冷却得快得多，目前冷却到大约2 × 10 8/sup/ K，但中子星星的热导率是这样的，至少需要几十年的时间才能使这种温度下降的影响到达中子星星的表面并被观察到。
Possible effects of strangeness condensation, which has been estimated to occur in dense neutron matter at densities of 2.3--3.0 times nuclear matter density, are calculated with special reference to the cooling of the neutron star probably formed in SN1987A. Although the center of the neutron star will cool much faster in the presence of strangeness condensation than through conventional mechanisms, down to Tapprox.2 x 10/sup 8/ K at the present time, the heat conductivity of the neutron star is such that it will take at least a few tens of years for effects of this drop in temperature to reach the surface of the neutron star and be observable.