Three-dimensional Magnetohydrodynamical Simulations of Gravitational Collapse of a 15 M [sun] Star
Three-dimensional Magnetohydrodynamical Simulations of Gravitational Collapse of a 15 M [sun] Star
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15 M [太阳] 恒星引力塌缩的三维磁流体动力学模拟
DOI：
10.1088/0067-0049/191/2/439
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发表时间：
2010
期刊：
影响因子：
--
通讯作者：
T. Kuroda and H. Umeda
中科院分区：
文献类型：
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作者：
吉田敬;梅田秀之;T. Kuroda and H. Umeda
我们介绍了我们的两个不同的新开发的，三维磁流体动力学的代码详细。其中一个是写在牛顿极限（NMHD），另一个是一个完全广义相对论代码（GRMHD）。这两个代码采用自适应网格细化，并在GRMHD中，该度量的演变与“鲍姆加特-夏皮罗-柴田-中村”的形式主义被称为目前最稳定的方法。我们进行了几个测试问题，作为第一个实际测试，我们计算了15 M星星的引力坍缩。计算结果表明：（1）在强磁化模型中，原中子星星驱动高速双极外流，并沿自转轴沿着运动;（2）出现单臂螺旋结构，起源于低磁化强度的|T/W|（3）通过比较GRMHD模型和NMHD模型，发现GRMHD模型中由于引力作用的增强，最大密度增加了约30%。这些特征与前人的研究结果吻合得很好，因此，我们的程序是可靠的大质量恒星引力坍缩的数值模拟。
We introduce our two different newly developed, three-dimensional magnetohydrodynamical codes in detail. One of them is written in the Newtonian limit (NMHD) and the other is a fully general relativistic code (GRMHD). Both codes employ adaptive mesh refinement and, in GRMHD, the metric is evolved with the" Baumgarte–Shapiro–Shibata–Nakamura" formalism known as the most stable method at present. We conducted several test problems and as for the first practical test, we calculated the gravitational collapse of a 15 M☉ star. The main features found from our calculations are:(1) high-velocity bipolar outflow is driven from the proto-neutron star and moves along the rotational axis in strongly magnetized models,(2) a one-armed spiral structure appears, which originates from the low-| T/W| instability, and (3) by comparing the GRMHD and NMHD models, the maximum density increases about∼ 30% in GRMHD models due to the stronger gravitational effect. These features agree very well with previous studies and our codes are thus reliable for numerical simulation of gravitational collapse of massive stars.