Magnetohydrodynamic (MHD) turbulence in neutron star (NS) merger remnants can impact their evolution and multimessenger signatures, complicating the interpretation of present and future observations. Due to the high Reynolds numbers and the large computational costs of numerical relativity simulations, resolving all the relevant scales of the turbulence will be impossible for the foreseeable future. Here, we adopt a method to include subgrid-scale turbulence in moderate resolution simulations by extending the large-eddy simulation (LES) method to general relativity (GR). We calibrate our subgrid turbulence model with results from very-high-resolution GRMHD simulations, and we use it to perform NS merger simulations and study the impact of turbulence. We find that turbulence has a quantitative, but not qualitative impact on the evolution of NS merger remnants, on their gravitational wave signatures, and on the outflows generated in binary NS mergers. Our approach provides a viable path to quantify uncertainties due to turbulence in NS mergers.

中文翻译：

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使用校准湍流模型的双中子星合并模拟

中子星 (NS) 并合残骸中的磁流体动力学 (MHD) 湍流会影响它们的演化和多信使特征，使当前和未来观测结果的解释复杂化。由于高雷诺数和数值相对论模拟的大量计算成本，在可预见的未来解决湍流的所有相关尺度是不可能的。在这里，我们采用了一种方法，通过将大涡模拟 (LES) 方法扩展到广义相对论 (GR)，在中等分辨率模拟中包含亚网格尺度湍流。我们使用来自超高分辨率 GRMHD 模拟的结果校准我们的子网格湍流模型，并使用它来执行 NS 合并模拟并研究湍流的影响。我们发现湍流有一个定量的，但对 NS 合并残余物的演化、它们的引力波特征以及二元 NS 合并产生的流出没有定性影响。我们的方法提供了一种可行的途径来量化由于 NS 合并中的湍流而导致的不确定性。