Analysing neutron star in HESS J1731-347 from thermal emission and cooling theory
Analysing neutron star in HESS J1731-347 from thermal emission and cooling theory
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DOI：
10.1093/mnras/stv2204
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发表时间：
2015-10
影响因子：
4.8
通讯作者：
D. Ofengeim;A. Kaminker;D. Klochkov;V. Suleimanov;D. Yakovlev
中科院分区：
文献类型：
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作者：
D. Ofengeim;A. Kaminker;D. Klochkov;V. Suleimanov;D. Yakovlev
超新星遗迹HESS J1731-347中的中央致密天体似乎是观测到的最热的孤立冷却中子星星。中子星的冷却理论使人们能够通过假设在恒星核心存在强质子超流性和存在几乎完全由碳组成的表面热覆盖层来解释对这颗星星的观测。该星星的冷却模型进行了阐述，以适当考虑中微子发射由于中子-中子碰撞，这是不抑制质子超流。利用3.2kpc距离下观测到的热谱的谱拟合结果和年龄为27 kyr的中子星星的冷却理论，得到了对恒星质量和半径的新的约束，这些约束比仅用谱拟合得到的约束更为严格。
The central compact object in the supernova remnant HESS J1731-347 appears to be the hottest observed isolated cooling neutron star. The cooling theory of neutron stars enables one to explain observations of this star by assuming the presence of strong proton superfluidity in the stellar core and the existence of the surface heat blanketing envelope which almost fully consists of carbon. The cooling model of this star is elaborated to take proper account of the neutrino emission due to neutron-neutron collisions which is not suppressed by proton superfluidity. Using the results of spectral fits of observed thermal spectra for the distance of 3.2 kpc and the cooling theory for the neutron star of age 27 kyr, new constraints on the stellar mass and radius are obtained which are more stringent than those derived from the spectral fits alone.