标题： 中子星合并中磁场增强的鲁棒性 显示英文标题

标题： Robustness of Magnetic Field Amplification in Neutron Star Mergers

摘要： 双中子星合并的动力学由在最极端条件下的物理规律所支配，包括强时空曲率、超高物质密度、明亮的中微子辐射以及初始中子星磁场的快速增强。 在这里，我们系统地探讨磁场均演化对合并双星总质量、组分质量比、恒星自转以及状态方程的敏感性。 为此，我们分析了16个最先进的GRMHD模拟，这些模拟采用亚网格尺度模型来考虑未解析的小尺度湍流。 我们发现，在高密度区域，磁场迅速增强至体积平均值为$\sim 10^{16}$~G 是中子星合并的一个非常稳健的结果，这一结果仅受到质量、质量比、自转或状态方程的轻微影响。 显示英文摘要

摘要： The dynamics of a binary neutron stars merger is governed by physics under the most extreme conditions, including strong spacetime curvature, ultra-high matter densities, luminous neutrino emission and the rapid amplification of the initial neutron star magnetic fields. Here we systematically explore how sensitive the magnetic field evolution is to the total mass of the merging binary, to the mass ratio of its components, the stellar spins and to the equation of state. For this purpose, we analyze 16 state-of-the-art GRMHD simulations that employ a subgrid-scale model to account for the unresolved small-scale turbulence. We find that strong and rapid amplification of the magnetic field to volume-averaged values of $\sim 10^{16}$~G in the high-density regions is a very robust outcome of a neutron star merger and this result is only marginally impacted by either mass, mass ratio, spin or equation of state.