SPECTRAL SCALING LAWS IN MAGNETOHYDRODYNAMIC TURBULENCE SIMULATIONS AND IN THE SOLAR WIND

被引：96

作者：

Boldyrev, Stanislav ^{[1
]}

Perez, Jean Carlos ^{[1
,2
,3
]}

Borovsky, Joseph E. ^{[4
,5
]}

Podesta, John J. ^{[4
]}

机构：

[1] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA

[2] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA

[3] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA

[4] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[5] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 741卷 / 01期

基金：

美国国家科学基金会;

关键词：

magnetic fields; magnetohydrodynamics (MHD); methods: statistical; plasmas; turbulence; NUMERICAL SIMULATIONS; WAVES;

D O I：

10.1088/2041-8205/741/1/L19

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The question is addressed as to what extent incompressible magnetohydrodynamics can describe random magnetic and velocity fluctuations measured in the solar wind. It is demonstrated that distributions of spectral indices for the velocity, magnetic field, and total energy obtained from high-resolution numerical simulations of magnetohydrodynamic turbulence are qualitatively and quantitatively similar to solar wind observations at 1 AU. Both simulations and observations show that in the inertial range the magnetic field spectrum E-b is steeper than the velocity spectrum E-v with E-b greater than or similar to E-v and that the magnitude of the residual energy E-R = E-v - E-b decreases nearly following a k(perpendicular to)(-2) scaling.

引用

页数：4

共 30 条

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