Superfluidity in Neutron Star Matter
Superfluidity in Neutron Star Matter
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DOI：
10.1007/3-540-44578-1_2
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发表时间：
2000-12
期刊：
影响因子：
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通讯作者：
U. Lombardo;H. Schulze
中科院分区：
文献类型：
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作者：
U. Lombardo;H. Schulze
中子物质超流性的研究可以追溯到Migdal的观察，即中子星是宏观超流系统的良好候选者[1]。事实上，在二十多年的中子-星星物理学中，中子和质子超流相的存在被用来解释中子星星的动力学和热演化。最引人注目的证据是由故障后的定时观测[2]，[3]给出的，但冷却历史也受到可能存在的超流体相的强烈影响[4]，[5]。在理论方面，在中子物质或更普遍的核物质背景下的超流性的开始在超导性的巴特尔，库珀和施里弗（BCS）理论[6]和原子核中的配对理论[7]，[8]形成后不久就被研究。
The research on the superfluidity of neutron matter can be traced back to Migdal’s observation that neutron stars are good candidates for being macroscopic superfluid systems [1]. And, in fact, during more than two decades of neutron-star physics the presence of neutron and proton superfluid phases has been invoked to explain the dynamical and thermal evolution of a neutron star. The most striking evidence is given by post-glitch timing observations [2],[3], but also the cooling history is strongly influenced by the possible presence of super- fluid phases [4],[5]. On the theoretical side, the onset of superfluidity in neutron matter or in the more general context of nuclear matter was investigated soon after the formulation of the Bardeen, Cooper, and Schrieffer (BCS) theory of superconductivity [6] and the pairing theory in atomic nuclei [7],[8].