标题： 大质量元素在旋转原磁星风中的合成 显示英文标题

标题： Heavy element nucleosynthesis in rotating proto-magnetar winds

摘要： 通过快速中子捕获过程（$r-$过程）合成的元素的天体物理起源是一个长期存在的谜题。 核心坍缩超新星的高温高密度环境被认为可能是$r-$过程的潜在发生地，尤其是新生原中子星（PNS）的中微子驱动风。 忽略PNS强磁场和/或快速旋转的潜在影响的风模型通常无法达到产生第三$r-$过程峰值的必要条件，但能稳健地产生有限或弱的$r-$过程对于富中子风。 具有磁星强度磁场的旋转和非旋转PNS风的轴对称磁流体动力学模拟显示，高熵物质从PNS磁层的赤道闭合区准周期性地喷射出来。 在此，我们使用核反应网络对这些模拟中的示踪粒子轨迹进行后处理，以探索不同PNS磁场强度、旋转速率和中微子光度（核心反弹后的冷却阶段）下的合成过程。 我们发现，即使磁场弱至$\sim 5\times 10^{14}$G，磁星形成过程中直到并超过第三个峰值的稳健$r-$过程是普遍存在的。根据初始磁场强度和自转的分布，我们估计磁化PNS风可以解释银河系$r-$过程库存的$\sim 5-100\%$，延伸到第三个峰值。我们计算中的稳健$r-$过程伴随着质量数为$\rm A\lesssim 120$的元素相对于太阳丰度的过量产生。 我们还发现，$^{92}\rm Mo$（一种$p-$同位素）在富中子风中大量产生。 显示英文摘要

摘要： The astrophysical origin of elements synthesized through the rapid neutron capture process ($r-$process) is a long standing mystery. The hot and dense environments of core-collapse supernovae have been suggested as potential $r-$process sites, particularly the neutrino-driven wind from the newly-born protoneutron star (PNS). Wind models that neglect the potential effects of strong magnetic fields and/or rapid rotation of the PNS typically fail to achieve the necessary conditions for production of the third $r-$process peak, but robustly produce a limited or weak $r-$process for neutron-rich winds. Axisymmetric magnetohydrodynamic simulations of rotating and non-rotating PNS winds with magnetar-strength fields reveal that high entropy material is quasi-periodically ejected from the equatorial closed zone of the PNS magnetosphere. Here, we post-process tracer particle trajectories from these simulations using a nuclear reaction network in order to explore the resulting nucleosynthesis across a range of PNS magnetic field strengths, rotation rates, and neutrino luminosities (cooling phase after core-bounce). We find that a robust $r-$process up to and beyond the third peak is generic to magnetar birth, even for magnetic fields as weak as $\sim 5\times 10^{14}$ G. Depending on the distribution of magnetic field strengths and rotation at birth, we estimate that magnetized PNS winds could account for $\sim 5-100\%$ of the Galactic $r-$process inventory, extending up to the third peak. The robust $r-$process in our calculations is accompanied by overproduction of elements with mass number $\rm A\lesssim 120$ compared to the Solar abundances. We also find that $^{92}\rm Mo$ (a $p-$isotope) is produced in significant quantities in neutron-rich winds.