An MHD Solar Wind Model with Turbulence Transport

被引：0

作者：

Usmanov, Arcadi V. ^{[1
,2
,3
]}

Matthaeus, William H. ^{[1
,2
]}

Breech, Ben ^{[3
]}

Goldstein, Melvyn L. ^{[3
]}

机构：

[1] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[2] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

[3] NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD USA

来源：

NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008 | 2009年 / 406卷

关键词：

ALFVEN WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; DISSIPATION; EVOLUTION;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present initial results from an axisymmetric steady-state solar wind model that describes properties of the large-scale solar wind, interplanetary magnetic field, and turbulence throughout the heliosphere from 0.3 AU to 100 AU. The model is based on numerical solutions of large-scale Reynolds-averaged magnetohydrodynamic (MHD) equations coupled with a set of small-scale transport equations for the turbulence energy, normalized cross-helicity, and correlation scale. The combined set of the time-dependent equations is solved in the frame of reference corotating with the Sun by a time-relaxation method. We use the model to study the global solar wind structure and the distribution of turbulence throughout the heliosphere.

引用

页码：160 / +

页数：3

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