从中子星致密性探测地壳结构
Probing crustal structures from neutron star compactness
摘要：
利用表征核物质状态方程的各种参数，我们系统地研究了中子星壳的厚度和其中所含的pasta相。然后，相对于球形核的相位的厚度，圆柱形的相位的厚度，和地壳厚度，我们成功地推导出拟合公式，表示每个厚度与恒星的半径作为一个函数的恒星的紧凑性，对称核物质的不可压缩性，和密度依赖的对称能量。特别地，我们发现球核的相厚度与地壳厚度一样，对恒星的致密性有很强的依赖性，但两者对状态方程参数的依赖性都要弱得多。因此，通过确定致密性，可以合理地限制球核相的厚度以及地壳厚度，即使EOS参数仍然是确定的。
英文摘要：
With various sets of the parameters that characterize the equation of state (EOS) of nuclear matter, we systematically examine the thickness of a neutron star crust and of the pasta phases contained therein. Then, with respect to the thickness of the phase of spherical nuclei, the thickness of the cylindrical phase, and the crust thickness, we successfully derive fitting formulas that express the ratio of each thickness to the star's radius as a function of the star's compactness, the incompressibility of symmetric nuclear matter, and the density dependence of the symmetry energy. In particular, we find that the thickness of the phase of spherical nuclei has such a strong dependence on the stellar compactness as the crust thickness, but both of them show a much weaker dependence on the EOS parameters. Thus, via determination of the compactness, the thickness of the phase of spherical nuclei as well as the crust thickness can be constrained reasonably, even if the EOS parameters remain to be well-determined.
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