This investigation explores the nucleonic thermal conductivity of nuclear star matter as it undergoes the “topological” transition to the “pasta” regime, and further down to the solid-liquid phase transition. The study was carried out using molecular dynamics simulations with nuclear potentials embedded in an effective (i.e. Thomas-Fermi) Coulomb potential. The nucleonic thermal conductivity experiences a dramatic change within a narrow temperature interval around $T\simeq 1$ MeV. This change accompanies the “pasta” breakdown during a heating process. The nucleonic thermal conductivity, by flipping protons' or neutrons' velocity, further shows a decoupling for asymmetric nuclear star matter.

这项研究探索了核星状物质经历“拓扑”过渡到“意大利面”状态，再到固-液相转变时的核子热导率。该研究是使用分子动力学模拟进行的，其中将核势嵌入有效（即Thomas-Fermi）库仑势中。核子的热导率在一个狭窄的温度区间内经历了巨大的变化$Ť\simeq \mathrm{1个}$MeV。这种变化伴随着加热过程中的“意大利面”击穿。通过翻转质子或中子的速度，核子的热导率进一步显示了非对称核星物质的解耦。