Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source

Employing phenomenological density-dependent critical temperatures of strong singlet-state proton pairing and of moderate triplet-state neutron pairing, we investigate the effects of rotochemical heating on the thermal evolution of superfluid neutron stars whose cores consist of npe matter with the Akmal-Pandharipande-Ravenhall equation of state. Since the star is not quite in the weak interaction equilibrium state during spin-down, the departure from the chemical equilibrium leads to the rotochemical heating in a rotating NS which will increase the stellar＇s temperature. Our calculations show that the rotochemical heating delays the cooling of superfluid neutron stars considerably and makes the previous classification of NS cooling ambiguous. What＇s more, our model is currently consistent with all the observational data, and in particular some middle-aged and cold NSs （PRS J0205＋6449 in 3C 58, PRS J1357-6429, RX J007.0＋7303 in CTA 1, Vela） can be better explained when taking into account rotochemical heating.     

准粒子描述下奇异夸克物质自洽热力学及对奇异星物态的影响

考虑夸克粒子间相互作用,研究了在准粒子近似下奇异夸克物质系统的热力学,发现由于热力学自洽的要求,需要在热力学势中额外增加一项.利用这一等效热力学讨论奇异夸克物质的物态方程及声速,得到了一个“软化”的物态,这与质量–密度相关模型是一致的.但准粒子描述模型能够显示介质效应对强相互作用耦合常数的依赖.     

高温近似下奇异夸克物质的体粘滞系数

在准粒子描述下,采用自洽的热力学方法,考虑奇异夸克物质(SQM?)的介质效应,计算了高温近似下奇异夸克物质的体粘滞系数.发现介质效应对奇异夸克物质的体粘滞系数有很大影响,这使得观测数据不再排除两味色超导相奇异星的存在.