Color superconductivity in compact stellar hybrid configurations
Color superconductivity in compact stellar hybrid configurations
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DOI：
10.1103/physrevc.96.065807
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发表时间：
2017-12
影响因子：
3.1
通讯作者：
I. F. Ranea-Sandoval;M. Orsaria;Sophia Han;F. Weber;W. Spinella
中科院分区：
文献类型：
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作者：
I. F. Ranea-Sandoval;M. Orsaria;Sophia Han;F. Weber;W. Spinella
质量约为2 M的恒星PSR J1614-2230和PSR J 0348 +0432的发现对冷的超致密物质的状态方程施加了强约束。如果从强子物质到夸克物质的相变发生在这种大质量中子星的内核，夸克物质的能量有利状态将是色超导体。在这项研究中，我们分析了此类中子星的稳定性和最大质量。强子相用非线性相对论平均场模型描述，夸克物质用局域Nambu-JonaLasinio模型描述。相变被视为麦克斯韦转变，假设一个尖锐的强子-夸克界面，和“恒定声速”（CSS）参数化讨论的存在下，恒星孪生配置。我们发现大质量中子星如J1614-2230和J 0348 +0432只能存在于连通的恒星分支上而不能存在于不连通的双星分支上。后者只能支持质量严格低于2 M质量的恒星。
The discovery of pulsars PSR J1614–2230 and PSR J0348+0432 with masses of around 2M ̄ imposes strong constraints on the equations of state of cold, ultradense matter. If a phase transition from hadronic matter to quark matter were to occur in the inner cores of such massive neutron stars, the energetically favorable state of quark matter would be a color superconductor. In this study, we analyze the stability and maximum mass of such neutron stars. The hadronic phase is described by nonlinear relativistic mean-field models, and the local Nambu-Jona Lasinio model is used to describe quark matter in the 2SC+s quark phase. The phase transition is treated as a Maxwell transition, assuming a sharp hadron-quark interface, and the “constant-sound-speed” (CSS) parametrization is employed to discuss the existence of stellar twin configurations. We find that massive neutron stars such as J1614-2230 and J0348+0432 can only exist on the connected stellar branch but not on the disconnected twin-star branch. The latter can only support stars with masses that are strictly below 2M ̄.