论文标题
Protoneutron Star对流模拟了新的一般相对论Boltzmann中微子辐射流动力学代码
Protoneutron Star Convection Simulated with a New General Relativistic Boltzmann Neutrino Radiation-Hydrodynamics Code
论文作者
论文摘要
我们使用我们新开发的一般相对论Boltzmann中微子辐射流动力学代码研究了原子恒星（PNS）对流。这是一项试点研究，供以后进行更全面的调查。因此，我们从1D PNS冷却计算中弹跳后2.3秒拍摄了PNS的快照，并在2D下以$ \ sim160 \，\ sim160 \，\ sim160 \，\ sim160 \，\ sim160 \，\ simrm {msationrm {MS} $在轴对称下的2D中。原始的PNS冷却计算完全忽略了对流，初始条件是线性不稳定的。在我们的2D模拟中，我们发现对流确实是在那里煽动的，并在被全面膨胀后向内扩展。然后将对流定位到$ \ sim100 \，\ mathrm {MS} $中的准稳态状态，由负$ y_e $梯度维持，而neutrino排放又可以维持。与1d相比，它增强了所有中微子的亮度和平均能量。利用Boltzmann求解器，我们分析了中微子快速风味转化率（FFC）的可能发生。我们发现FFC可能发生在$ y_e $较低的区域中，并且增长率可以高达$ \ sim 10^{ - 1} \，{\ Mathrm {cm}^{ - 1}}} $。
We investigate the protoneutron star (PNS) convection using our newly developed general relativistic Boltzmann neutrino radiation-hydrodynamics code. This is a pilot study for more comprehensive investigations later. As such, we take a snapshot of a PNS at 2.3 seconds after bounce from a 1D PNS cooling calculation and run our simulation for $\sim160\,\mathrm{ms}$ in 2D under axisymmetry. The original PNS cooling calculation neglected convection entirely and the initial condition is linearly unstable to convection. We find in our 2D simulation that convection is instigated there indeed and expands inward after being full-fledged. The convection is then settled to a quasi-steady state in $\sim100\,\mathrm{ms}$, being sustained by the negative $Y_e$ gradient, which is in turn maintained by neutrino emissions. It enhances the luminosities and mean energies of all species of neutrinos compared to 1D. Taking advantage of the Boltzmann solver, we analyze the possible occurrence of the neutrino fast flavor conversion (FFC). We found that FFC is likely to occur in the regions, where $Y_e$ is lower, and that the growth rate can be as high as $\sim 10^{-1}\,{\mathrm{cm}^{-1}}$.
