Mach Number Dependence of Turbulent Magnetic Field Amplification: Solenoidal versus Compressive Flows

被引：211
作者：
Federrath, C. [1 ,3 ]
Chabrier, G. [1 ,2 ]
Schober, J. [3 ]
Banerjee, R. [4 ]
Klessen, R. S. [3 ]
Schleicher, D. R. G. [5 ]
机构：
[1] Ecole Normale Super Lyon, F-69364 Lyon, France
[2] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England
[3] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany
[4] Hamburger Sternwarte, D-21029 Hamburg, Germany
[5] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany
来源：
PHYSICAL REVIEW LETTERS | 2011年 / 107卷 / 11期
关键词：
INTERSTELLAR TURBULENCE; ISOTHERMAL TURBULENCE; DYNAMO ACTION; 1ST STARS; SIMULATIONS; MAGNETOHYDRODYNAMICS; STATISTICS; GALAXIES; GAS; I;
D O I：
10.1103/PhysRevLett.107.114504
中图分类号：
O4 [物理学];
学科分类号：
0702 ;
摘要：
We study the growth rate and saturation level of the turbulent dynamo in magnetohydrodynamical simulations of turbulence, driven with solenoidal (divergence-free) or compressive (curl-free) forcing. For models with Mach numbers ranging from 0.02 to 20, we find significantly different magnetic field geometries, amplification rates, and saturation levels, decreasing strongly at the transition from subsonic to supersonic flows, due to the development of shocks. Both extreme types of turbulent forcing drive the dynamo, but solenoidal forcing is more efficient, because it produces more vorticity.
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页数：5
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