论文标题
手性意大利面
Chiral pasta
论文作者
论文摘要
中子恒星的内部是超密集的，可能包含脱合夸克物质的核心。这样的核心可以平稳地连接到外层或通过尖锐的显微镜界面或通过中间混合相的中间宏观层连接到全球中性，但本地包含电动域。在这里，我在中子恒星条件下采用核素 - 梅森模型，该模型在大密度下显示了一阶手性相变。在此手性转变附近，我计算了Wigner -Seitz近似中各种混合相的自由能 - 不同的“面食结构”。至关重要的是，在同一基础上处理了手性折断的核物质和大约手智的对称相（松散解释为夸克物质）。这使我能够完全始终如一地计算气泡，杆和平板的界面曲线，并考虑电磁筛选效果，而无需表面张力作为输入。我发现，与文献中经常使用的简单阶梯状近似相比，完整的数值结果倾向于不利于混合阶段，并且主要偏爱的面食结构由具有表面张力$σ\ simeq 6 \，{\ rm mev}/{\ rm mev}/{\ rm fm fm fm}^2 $组成。
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 $Σ\simeq 6\, {\rm MeV}/{\rm fm}^2$.
