NUMERICAL SIMULATIONS OF DRIVEN RELATIVISTIC MAGNETOHYDRODYNAMIC TURBULENCE
NUMERICAL SIMULATIONS OF DRIVEN RELATIVISTIC MAGNETOHYDRODYNAMIC TURBULENCE
复制标题
驱动相对论磁流体湍流的数值模拟
DOI：
10.1088/0004-637x/744/1/32
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
A. MacFadyen
中科院分区：
文献类型：
--
作者：
J. Zrake;A. MacFadyen
各种各样的天体物理现象涉及具有相对论速度或能量密度的湍流磁化气体的流动。例子包括伽玛射线暴、活动星系核、类星体、磁星、微类星体、合并中子星、X射线双星、一些超新星和早期宇宙。为了阐明这些系统中存在的相对论磁流体动力学（RMHD）湍流的基本性质，我们提出了充分发展的驱动湍流在相对论温暖，弱磁化和温和的可压缩理想流体的数值模拟结果。我们使用高阶Godunov代码在具有10243个区域的均匀网格上演化了许多动态时间的RMHD方程。我们观察到的增长的磁能从种子场通过饱和在总流体能量的0.1%。我们计算了速度和密度加权速度U = ρ1/3v的功率谱，并得出结论，惯性标度与-5/3的斜率一致。我们计算的纵向和横向速度结构函数的顺序p到11，并讨论他们可能偏离预期的非相对论介质的标度。我们还计算了相干速度结构相对于局部磁场的尺度依赖性失真，找到了一个较弱的尺度依赖性比预期的不可压缩的非相对论流与强平均场。
A wide variety of astrophysical phenomena involve the flow of turbulent magnetized gas with relativistic velocity or energy density. Examples include gamma-ray bursts, active galactic nuclei, pulsars, magnetars, micro-quasars, merging neutron stars, X-ray binaries, some supernovae, and the early universe. In order to elucidate the basic properties of the relativistic magnetohydrodynamical (RMHD) turbulence present in these systems, we present results from numerical simulations of fully developed driven turbulence in a relativistically warm, weakly magnetized and mildly compressible ideal fluid. We have evolved the RMHD equations for many dynamical times on a uniform grid with 10243 zones using a high-order Godunov code. We observe the growth of magnetic energy from a seed field through saturation at ∼1% of the total fluid energy. We compute the power spectrum of velocity and density-weighted velocity U = ρ1/3v and conclude that the inertial scaling is consistent with a slope of −5/3. We compute the longitudinal and transverse velocity structure functions of order p up to 11 and discuss their possible deviation from the expected scaling for non-relativistic media. We also compute the scale-dependent distortion of coherent velocity structures with respect to the local magnetic field, finding a weaker scale dependence than is expected for incompressible non-relativistic flows with a strong mean field.
DOI：
10.1088/0067-0049/193/1/6
发表时间：
2011-01
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
K. Beckwith;J. Stone
通讯作者：
K. Beckwith;J. Stone
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell