General-relativistic resistive-magnetohydrodynamic simulations of binary neutron stars
General-relativistic resistive-magnetohydrodynamic simulations of binary neutron stars
复制标题
双中子星的广义相对论电阻磁流体动力学模拟
DOI：
10.1103/physrevd.92.084064
复制
发表时间：
2015
影响因子：
5
通讯作者：
L. Rezzolla
中科院分区：
文献类型：
--
作者：
K. Dionysopoulou;D. Alic;L. Rezzolla
我们已经研究了一个等质量磁化中子星二进制内的电阻磁流体动力学（RMHD）的方法，在该方法中，高导电的恒星内部是匹配的电真空外部的动力学。因为我们的分析是为了评估合并后的动态二进制的电阻效应，并通过崩溃引入的修改，我们进行了密切的比较与传统的理想磁流体动力学近似内进行的等效模拟。我们发现这两种演化有许多相似之处，但也有一个重要的区别：超大质量中子星星的生存时间在RMHD模拟中增加。这种差异是由于在电阻机制中效率较低的磁制动机制，其中物质可以穿过磁场线移动，从而减少了角动量的向外传输。本文所进行的RMHD和理想磁流体动力学模拟都是在比我们以前的工作更高的分辨率和不同的网格结构下进行的[L。雷佐拉，B。贾科马佐湖Baiotti，J. Granot，C. Kouveliotou和M. A.阿洛伊，太空人。J. Letters 732，L 6（2011）]，但证实了低密度漏斗的形成，其具有由黑洞-环面系统产生的有序磁场。在这两个制度的磁场主要是环形的高导电环和主要极向在近真空漏斗。在漏斗中发生的重新连接过程或中微子湮灭，我们没有一个模型，可能会增加漏斗中的内部能量，并发射相对论性外流，然而，在这些模拟中没有产生。
We have studied the dynamics of an equal-mass magnetized neutron-star binary within a resistive magnetohydrodynamic (RMHD) approach in which the highly conducting stellar interior is matched to an electrovacuum exterior. Because our analysis is aimed at assessing the modifications introduced by resistive effects on the dynamics of the binary after the merger and through to collapse, we have carried out a close comparison with an equivalent simulation performed within the traditional ideal magnetohydrodynamic approximation. We have found that there are many similarities between the two evolutions but also one important difference: the survival time of the hypermassive neutron star increases in a RMHD simulation. This difference is due to a less efficient magnetic-braking mechanism in the resistive regime, in which matter can move across magnetic-field lines, thus reducing the outward transport of angular momentum. Both the RMHD and the ideal magnetohydrodynamic simulations carried here have been performed at higher resolutions and with a different grid structure than those in previous work of ours [L. Rezzolla, B. Giacomazzo, L. Baiotti, J. Granot, C. Kouveliotou, and M. A. Aloy, Astrophys. J. Letters 732, L6 (2011)] but confirm the formation of a low-density funnel with an ordered magnetic field produced by the black hole-torus system. In both regimes the magnetic field is predominantly toroidal in the highly conducting torus and predominantly poloidal in the nearly evacuated funnel. Reconnection processes or neutrino annihilation occurring in the funnel, none of which we model, could potentially increase the internal energy in the funnel and launch a relativistic outflow, which, however, is not produced in these simulations.
剪切粒子系统中剪切应力的时间相关函数
DOI：
--
发表时间：
2009
期刊：
Progress of Theoretical Physics, Supplement 178
影响因子：
--
作者：
T. Sakai;他;Hiroto Kuninaka,and Hisao Hayakawa;Michio Otsuki,and Hisao Hayakawa;Michio Otsuki,and Hisao Hayakawa;Hisao Hayakawa,and Michio Otsuki;Michio Otsuki,and Hisao Hayakawa
通讯作者：
Michio Otsuki,and Hisao Hayakawa