双中子星并合中的输运性质：磁场的影响
Transport properties in binary neutron star mergers: Effect of magnetic field
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中文总结 AI 辅助
该研究针对双中子星并合的极端环境，提出有限温度与磁场下计算带电流Urca发射率和中微子不透明度的精确框架，发现极端磁场会显著增强中微子不透明度，缩短热中微子平均自由程。
中文摘要 AI 辅助
在双中子星并合这类极端环境中，温度可高达50 MeV，磁场强度可达10^17 G，此时中微子输运主导宏观热力学与化学演化。现有并合模拟采用零磁场下的中微子发射率与不透明度，可能遗漏高磁化中子星核心的关键输运物理。我们提出了一个有限温度与磁场下计算带电流Urca发射率和中微子不透明度的精确框架，采用Nucleon Width Approximation框架考虑高密度核心主导的碰撞展宽效应。计算表明，极端磁场会显著增强带电流中微子不透明度，有效缩短热中微子的平均自由程。
英文摘要
In extreme environments such as binary neutron star mergers, temperatures as high as $50$ MeV and magnetic fields up to $10^{17}$ G, reach a regime where neutrino transport governs the macroscopic thermodynamic and chemical evolution. Existing merger simulations rely on zero magnetic field neutrino emissivity and opacity, potentially missing critical transport physics in highly magnetized neutron star cores. We present an exact framework for computing charged current Urca emissivity and neutrino opacity at finite temperature and magnetic field. We employ the Nucleon Width Approximation framework to account for the collisional broadening effects dominant in the high-density core. Our calculations demonstrate that extreme magnetic fields significantly enhance charged current neutrino opacity, effectively reducing the mean free path for thermal neutrinos.
