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

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【作者】 皮春梅杨书华周霞周爱芝

【Author】 PI Chun-Mei 1 , 2 YANG Shu-Hua 1 ZHOU Xia 3 ZHOU Ai-Zhi 1 1 Institute of Astrophysics, Huazhong Normal University, Wuhan 430079, China 2 Department of Physics and Electronics, Hubei University of Education, Wuhan 430205, China 3 Urumqi Observatory, NAOC, CAS, 40-5 South BeiJiang Road, Urumqi 830011, China

【机构】 Institute of Astrophysics, Huazhong Normal UniversityDepartment of Physics and Electronics, Hubei University of EducationUrumqi Observatory, NAOC, CAS

【摘要】 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 spindown, 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.

【Abstract】 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 spindown, 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.

【基金】 Supported by National Natural Science Foundation of China (10603002, 10773004);Western Light Talent Culture Project of Chinese Academy of Sciences (XBBS200920)
  • 【文献出处】 中国物理C ,Chinese Physics C , 编辑部邮箱 ,2010年12期
  • 【分类号】P145.6
  • 【下载频次】17
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