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arXiv 2002.01451hep-phastro-ph.HEnucl-th
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手性面食

Chiral pasta

Andreas Schmitt

备注：
19 pages, 8 figures; v2: minor improvements in the text, one reference added, accepted for publication in Phys. Rev. D
发表信息：
Phys. Rev. D 101, 074007 (2020)
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摘要：

中子星的内部是超致密的，可能包含一个非限定夸克物质的核心。这样的核心平滑地或通过尖锐的微观界面或通过不均匀混合相的中间宏观层连接到外层，所述中间宏观层是全局中性的，但局部包含带电域。在这里，我采用了中子星条件下的核子介子模型，显示了在大密度的一阶手征相变。在附近的手性过渡，我计算的自由能的各种混合相-不同的“面食结构”-在维格纳-塞茨近似。重要的是，手征破缺的核物质和近似手征对称的相（广义上解释为夸克物质）是在同一个基础上处理的。这使我能够计算气泡，棒和板的界面轮廓完全一致，考虑到电磁屏蔽效应，而不需要表面张力作为输入。我发现，完整的数值结果往往不利于混合相相比，在文献中经常使用的一个简单的阶梯状近似，主要青睐的面食结构由具有表面张力$Σ\simeq 6\, {\rm MeV}/{\rm fm}^2$的板坯。

英文摘要：

Interiors of neutron stars are ultra-dense and may contain a core of deconfined quark matter. Such a core connects to the outer layers smoothly or through a sharp microscopic interface or through an intermediate macroscopic layer of inhomogeneous mixed phases, which is globally neutral but locally contains electrically charged domains. Here I employ a nucleon-meson model under neutron star conditions that shows a first-order chiral phase transition at large densities. In the vicinity of this chiral transition I calculate the free energies of various mixed phases - different 'pasta structures' - in the Wigner-Seitz approximation. Crucially, chirally broken nuclear matter and the approximately chirally symmetric phase (loosely interpreted as quark matter) are treated on the same footing. This allows me to compute the interface profiles of bubbles, rods, and slabs fully consistently, taking into account electromagnetic screening effects and without needing the surface tension as an input. I find that the full numerical results tend to disfavor mixed phases compared to a simple step-like approximation used frequently in the literature and that the predominantly favored pasta structure consists of slabs with a surface tension $Σ\simeq 6\, {\rm MeV}/{\rm fm}^2$.

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