Hadron-quark crossover and massive hybrid stars
Hadron-quark crossover and massive hybrid stars
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DOI：
10.1093/ptep/ptt045
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发表时间：
2012-12
影响因子：
3.5
通讯作者：
Kota Masuda;T. Hatsuda;T. Takatsuka
中科院分区：
文献类型：
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作者：
Kota Masuda;T. Hatsuda;T. Takatsuka
基于从超子强子相到奇异夸克相的渗流图象，我们构造了一个新的状态方程，该方程的压力插值为重子密度的函数。中子星的最大质量可以超过2 M_{\odot }$，如果满足以下两个条件：（i）强子物质到夸克物质的跃迁发生在正常核物质密度的三倍左右，（ii）夸克物质在跃迁区域有强相互作用，并具有刚性状态方程。这与传统的方法相反，假设一阶相变，其中由于高密度夸克物质的存在，EOS总是变得柔软。虽然强子物态方程的选择并不影响最大质量的上述结论，但核子和超子之间的三体力在超子混合的开始和中子星的冷却中起着至关重要的作用。
On the basis of the percolation picture from the hadronic phase with hyperons to the quark phase with strangeness, we construct a new equation of state (EOS) with the pressure interpolated as a function of the baryon density. The maximum mass of neutron stars can exceed $2M_{\odot }$ if the following two conditions are satisfied: (i) the crossover from hadronic matter to quark matter takes place at around three times the normal nuclear matter density, and (ii) the quark matter is strongly interacting in the crossover region and has a stiff equation of state. This is in contrast to the conventional approach, assuming the first-order phase transition in which the EOS always becomes soft due to the presence of the quark matter at high density. Although the choice of the hadronic EOS does not affect the above conclusion for the maximum mass, the three-body force among nucleons and hyperons plays an essential role in the onset of hyperon mixing and the cooling of neutron stars.