SIMULATION STUDY OF A MAGNETOHYDRODYNAMIC DYNAMO - CONVECTION IN A ROTATING SPHERICAL-SHELL

被引：23

作者：

KAGEYAMA, A ^{[1
]}

WATANABE, K ^{[1
]}

SATO, T ^{[1
]}

机构：

[1] HIROSHIMA UNIV,FAC SCI,HIROSHIMA 724,JAPAN

来源：

PHYSICS OF FLUIDS B-PLASMA PHYSICS | 1993年 / 5卷 / 08期

基金：

美国国家卫生研究院;

关键词：

D O I：

10.1063/1.860668

中图分类号：

O35 [流体力学]; O53 [等离子体物理学];

学科分类号：

070204 ; 080103 ; 080704 ;

摘要：

Numerical simulations on the thermal convection of a neutral fluid (without a magnetic field) in a rotating spherical shell have been carried out. The results indicate that sufficiently rapid rotation results in strong differential rotation, with a pronounced equatorial acceleration. The formation dynamics of convection columns aligned to the rotation axis is studied extensively. A new generation mechanism of differential rotation is then proposed which concludes that the fluid motion generates an equatorial acceleration by selectively exciting the cyclonic columns in the spherical shell.

引用

页码：2793 / 2805

页数：13

共 31 条

[1]

Busse F., 1977, GEOPHYSICAL ASTROPHY, V8, P17, DOI [10.1080/03091927708240369, DOI 10.1080/03091927708240369]

[2] DIFFERENTIAL ROTATION IN STELLAR CONVECTION ZONES [J].