In this review we study the nuclear pastas as they are expected to be formed in neutron star crusts. We start with a study of the pastas formed in nuclear matter (composed of protons and neutrons), we follow with the role of the electron gas on the formation of pastas, and we then investigate the pastas in neutron star matter (nuclear matter embedded in an electron gas).

Nuclear matter (NM) at intermediate temperatures (1 MeV ≲ T ≲ 15 MeV), at saturation and sub-saturation densities, and with proton content ranging from 30% to 50% was found to have liquid, gaseous and liquid-gas mixed phases. The isospin-dependent phase diagram was obtained along with the critical points, and the symmetry energy was calculated and compared to experimental data and other theories. At low temperatures (T ≲ 1 MeV) NM produces crystal-like structures around saturation densities, and pasta-like structures at sub-saturation densities. Properties of the pasta structures were studied with cluster-recognition algorithms, caloric curve, the radial distribution function, the Lindemann coefficient, Kolmogorov statistics, Minkowski functionals; the symmetry energy of the pasta showed a connection with its morphology.

Neutron star matter (NSM) is nuclear matter embedded in an electron gas. The electron gas is included in the calculation by the inclusion of an screened Coulomb potential. To connect the NM pastas with those in neutron star matter (NSM), the role the strength and screening length of the Coulomb interaction have on the formation of the pastas in NM was investigated. Pasta was found to exist even without the presence of the electron gas, but the effect of the Coulomb interaction is to form more defined pasta structures, among other effects. Likewise, it was determined that there is a minimal screening length for the developed structures to be independent of the cell size.

Neutron star matter was found to have similar phases as NM, phase transitions, symmetry energy, structure function and thermal conductivity. Like in NM, pasta forms at around T ≈ 1.5 MeV, and liquid-to-solid phase changes were detected at T ≈ 0.5 MeV. The structure function and the symmetry energy were also found to depend on the pasta structures.

在这篇综述中，我们研究了预期在中子星外壳中形成的核面食。我们首先研究核物质（由质子和中子组成）中形成的面食，然后研究电子气在面食形成中的作用，然后研究中子星状物质（内含核物质）中的面食。电子气）。

在中间温度核物质（NM）（1MeV的≲ Ť在饱和和次饱和密度下，质子含量在30％至50％的范围内（约15 MeV）被发现具有液态，气态和液气混合相。获得了与同位旋有关的相图以及临界点，并计算了对称能，并将其与实验数据和其他理论进行了比较。在低温（T≲1 MeV）下，NM在饱和密度附近产生晶体状结构，在亚饱和密度下产生面食状结构。使用聚类识别算法，热量曲线，径向分布函数，Lindemann系数，Kolmogorov统计量，Minkowski泛函来研究面食结构的特性；面食的对称能量与其形态有关。

中子星物质（NSM）是嵌入电子气中的核物质。通过包括屏蔽的库仑电势将电子气包括在计算中。为了将NM面食与中子星物质（NSM）中的面食连接起来，研究了库仑相互作用的强度和筛选长度对NM面食形成的作用。发现面食甚至在不存在电子气的情况下也存在，但是库仑相互作用的作用是形成更明确的面食结构，以及其他作用。同样，已确定对于展开的结构，其最小筛选长度与细胞大小无关。

发现中子星物质具有与NM相类似的相，相变，对称能，结构函数和热导率。像在NM，在面食形成围绕Ť ≈1.5兆电子伏特，和液-固相变化检测在Ť ≈0.5兆电子伏。还发现结构功能和对称能量取决于面食结构。