标题： 中子星中核面团形成的填充分数：半经典预测与液滴模型预测 显示英文标题

标题： Filling fractions for the formation of nuclear pasta in neutron stars: semiclassical vs liquid-drop predictions

摘要： 历史上，在中子星内壳层最深处的可压缩液滴模型中预测了一连串的核意大利面结构形状会出现，当填充分数$u$超过某些阈值时。 然而，后来的计算表明这些值取决于液滴模型的细节。 在这里，我们使用各种广义Skyrme泛函在半经典扩展的Thomas-Fermi方法中研究了中子星中的意大利面结构的存在性。 发现不同转变的填充分数是准普遍的，与受控于相关密度下对称能的意大利面密度范围不同。 特别是，意大利面结构出现在$u_\mathrm{sp}\approx0.13-0.15$时。 通过在液滴框架内应用一个简化的稳定性标准，我们证明这些值 $u_\mathrm{sp}$可以用核曲率校正来解释。 这样，意大利面结构的丰度可以很容易地估计出来。 这个标准也可以用来优化在更现实的扩展 Thomas-Fermi方法中寻找意大利面结构。 显示英文摘要

摘要： Historically, a sequence of nuclear pasta shapes was predicted to appear in the deepest region of the inner crust of a neutron star within the compressible liquid-drop picture, when the filling fraction $u$ exceeds some threshold values. However, later calculations showed that these values depend on the details of the liquid-drop model. Here we investigate the existence of pasta in neutron stars within the semiclassical extended Thomas-Fermi approach using various generalized Skyrme functionals. The filling fractions for the different transitions are found to be quasi-universal, unlike the pasta density ranges governed by the symmetry energy at relevant densities. In particular, pasta emerge at $u_\mathrm{sp}\approx0.13-0.15$. By applying a simplified stability criterion within the liquid-drop framework, we show that these values of $u_\mathrm{sp}$ can be explained by the nuclear curvature correction. In this way, the abundance of pasta can be easily estimated. This criterion can also be used to optimize the search of pasta within the more realistic extended Thomas-Fermi approach.