Nuclear Impurities in the Superfluid Crust of Neutron Stars: Quantum Calculation and Observable Effects on the Cooling
Nuclear Impurities in the Superfluid Crust of Neutron Stars: Quantum Calculation and Observable Effects on the Cooling
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中子星超流壳中的核杂质：量子计算和对冷却的可观察影响
DOI：
10.1086/339284
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
R. Broglia
中科院分区：
文献类型：
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作者：
P. Pizzochero;F. Barranco;E. Vigezzi;R. Broglia
我们进行量子力学计算的中子比热的魏格纳-塞茨细胞的特点的内壳的中子星星，在库仑晶格的中子丰富的核是由海洋的未结合的超流中子渗透。然后，我们评估与这样的微观结构相关的可观察到的热性质，并将它们与在没有核杂质的地壳超流性的均匀密度模型中获得的标准值进行比较。我们首先认为，热扩散的瓶颈是由内地壳的最外层代表。然后，我们表明，获得的非均匀系统的地壳冷却时间是显着不同的标准的均匀模型。我们发现，这种差异的符号和大小敏感地依赖于当地的物质温度和对势。我们的结论是，为了给预测的权力，从中子星的热发射观测，它是至关重要的，包括在任何现实的冷却代码的核杂质的影响，中子超流体。
We perform a quantum mechanical calculation of the neutron-specific heat in the Wigner-Seitz cells that characterize the inner crust of a neutron star, where a Coulomb lattice of neutron-rich nuclei is permeated by a sea of unbound superfluid neutrons. We then evaluate the observable thermal properties associated with such a microscopic structure and compare them to the standard values obtained in a uniform density model of the crust superfluidity with no nuclear impurities. We first argue that the bottleneck for the diffusion of heat is represented by the outermost layers of the inner crust. We then show that the crust-cooling times obtained for the nonuniform system are significantly different from those obtained in the standard uniform model. We find that the sign and magnitude of this difference depend sensitively on the local matter temperature and the pairing potential. We conclude that in order to give predictive power to observations of the thermal emission from neutron stars, it is crucial to include in any realistic cooling code the effect of nuclear impurities on the neutron superfluid.
影响因子：
1.4
作者：
DOBACZEWSKI, J;FLOCARD, H;TREINER, J
通讯作者：
TREINER, J
N. Itoh：“恒星内部的中微子能量损失。VII。”
DOI：
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