具有夸克核的快速旋转轴对称中子星
Rapidly rotating axisymmetric neutron stars with quark cores
摘要：
本文系统地研究了纯强子和混合致密星的性质。利用密度相关的有效核子-核子相互作用，在满足重离子碰撞流场观测数据的约束条件下，得到了β平衡中子星物质的核物质状态方程.夸克物质的能量密度低于高密度时的核EoS，这意味着核内有可能发生向夸克物质的转变。我们用纯核物质和夸克核求解了旋转恒星的爱因斯坦方程。具有薄壳的β平衡中子星物质能够描述高质量的致密星，但发现中子星内部的核到夸克物质的解除禁闭跃迁导致它们的质量减少。J1614-2230毫秒脉冲双星的最新观测。Demorest等人[1]认为质量在1.97 \pm 0.04 M \odot范围内，其中M \odot是太阳质量。与最近的观测结果一致，纯核子EoS确定了以低于r模不稳定性的频率旋转的NS的最大质量为~1.95 M \odot，半径为~10 km。虽然具有以开普勒频率旋转的夸克核的致密恒星的质量高达~2 M \odot，但如果最大频率受到r模式不稳定性的限制，最大质量~1.7 M \odot将低于观测到的质量1.97 \pm 0.04 M \odot，这是迄今为止测量到的最高质量，这意味着这种大质量的夸克不包括夸克核。
英文摘要：
We present a systematic study of the properties of pure hadronic and hybrid compact stars. The nuclear equation of state (EoS) for beta-equilibrated neutron star matter was obtained using density dependent effective nucleon-nucleon interaction which satisfies the constraints from the observed flow data from heavy-ion collisions. The energy density of quark matter is lower than that of this nuclear EoS at higher densities implying the possibility of transition to quark matter inside the core. We solve the Einstein's equations for rotating stars using pure nuclear matter and quark core. The beta- equilibrated neutron star matter with a thin crust is able to describe highly massive compact stars but find that the nuclear to quark matter deconfinement transition inside neutron stars causes reduction in their masses. Recent observations of the binary millisecond pulsar J1614-2230 by P. B. Demorest et al. [1] suggest that the masses lie within 1.97\pm0.04 M\odot where M\odot is the solar mass. In conformity with recent observations, pure nucleonic EoS determines that the maximum mass of NS rotating with frequency below r-mode instability is ~1.95 M\odot with radius ~10 kilometers. Although compact stars with quark cores rotating with Kepler's frequency have masses up to ~2 M\odot, but if the maximum frequency is limited by the r-mode instability, the maximum mass ~1.7 M\odot turns out to be lower than the observed mass of 1.97\pm0.04 M\odot, by far the highest yet measured with such certainty, implying exclusion of quark cores for such massive pulsars.
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