恒星中韧致辐射中微子发射的光谱和速率
Spectra and rates of bremsstrahlung neutrino emission in stars
摘要：
考虑到电子屏蔽和离子关联的影响，我们计算了恒星内部电子核韧致辐射中微子发射的能量微分率。我们比较的能量微分和净率，以及平均$\barν_e$和$\barν_x$ $(x = μ, τ)$能量，这个过程与那些$e^{\pm}$对湮灭，等离子体衰变，光中微子发射在很宽的温度和密度范围。我们还比较了我们更新的能量损失率为上述热中微子发射过程中广泛使用的拟合公式在恒星演化模型，并确定温度和密度域中，每个过程占主导地位。我们讨论了我们的研究结果的影响，从大质量的恒星在其前超新星的演化过程中检测$\barν_e$，发现对湮灭的热发射过程中的信号作出了主要贡献。
英文摘要：
We calculate the energy-differential rate for neutrino emission from electron-nucleus bremsstrahlung in stellar interiors taking into account the effects of electron screening and ionic correlations. We compare the energy-differential and the net rates, as well as the average $\barν_e$ and $\barν_x$ $(x = μ, τ)$ energies, for this process with those for $e^{\pm}$ pair annihilation, plasmon decay, and photo-neutrino emission over a wide range of temperature and density. We also compare our updated energy loss rates for the above thermal neutrino emission processes with the fitting formulas widely used in stellar evolution models and determine the temperature and density domain in which each process dominates. We discuss the implications of our results for detection of $\barν_e$ from massive stars during their pre-supernova evolution and find that pair annihilation makes the predominant contribution to the signal from the thermal emission processes.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
