Nuclear pasta in hot dense matter and its implications for neutrino scattering
Nuclear pasta in hot dense matter and its implications for neutrino scattering
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DOI：
10.1103/physrevc.97.045804
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发表时间：
2017-10
影响因子：
3.1
通讯作者：
A. Roggero;J. Margueron;L. Roberts;S. Reddy
中科院分区：
文献类型：
--
作者：
A. Roggero;J. Margueron;L. Roberts;S. Reddy
我们发现当物质接近β平衡时，有限温度效应会大大降低亚核密度下富中子物质中大核子团簇的丰度。大核和异国情调的非球形核配置称为面食，有利于在附近的过渡到均匀的物质在T=0$，溶解在相对较低的温度。对于接近β平衡的物质，我们发现对于现实的状态方程，面食熔化温度为$T_m^\beta\simeq 4\pm 1$~MeV。面食溶解的机制进行了讨论，并在一般情况下，T_m^\beta$被证明是敏感的质子分数。我们发现，相干中微子散射的核和面食作出适度的贡献，在超新星和中子星星合并遇到的条件下的不透明度。银河系超新星中微子信号的影响进行了简要讨论。
We find that the abundance of large clusters of nucleons in neutron-rich matter at sub-nuclear density is greatly reduced by finite temperature effects when matter is close to beta-equilibrium. Large nuclei and exotic non-spherical nuclear configurations called pasta, favored in the vicinity of the transition to uniform matter at $T=0$, dissolve at relatively low temperature. For matter close to beta-equilibrium we find that the pasta melting temperature is $T_m^\beta\simeq 4\pm 1$~MeV for realistic equations of state. The mechanism for pasta dissolution is discussed, and in general $T_m^\beta$ is shown to be sensitive to the proton fraction. We find that coherent neutrino scattering from nuclei and pasta makes a modest contribution to the opacity under the conditions encountered in supernovae and neutron star mergers. Implications for neutrino signals from galactic supernovae are briefly discussed.