TURBULENCE IN A ROTATING MAGNETIZED FLUID

被引：1

作者：

PIPIN, VV ^{[1
]}

机构：

[1] SOLAR TERRESTRIAL PHYS INST, IRKUTSK 664033, RUSSIA

来源：

ASTRONOMISCHE NACHRICHTEN | 1994年 / 315卷 / 02期

关键词：

ROTATING MAGNETIZED FLUID; TURBULENCE;

D O I：

10.1002/asna.2103150204

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In a quasilinear approximation, for a special model of initial turbulence the combined effect of the rotation and the large-scale toroidal magnetic field was calculated. For large values of parameters of magnetic field strength and rotation rate the intensity of turbulent motions is suppressed in inverse proportion to the product of a mean magnetic field strength and the rotation rate of the medium. With increasing magnetic field strength and rotation rate. the inhomogeneity scale of turbulence increases in the direction of both the magnetic field and the angular velocity vector.

引用

页码：151 / 156

页数：6

共 10 条

[1]

CANUTO VM, 1986, ASTRON ASTROPHYS, V168, P89

[2]

KITCHATINOV LL, 1991, ASTRON ASTROPHYS, V243, P483

[3]

Krause F., 1980, MEAN FIELD MAGNETOHY

[4]

MILNETHOMSON LM, 1964, HDB MATH FUNCTIONS, P380

[5]

PARKER EN, 1979, COSMICAL MAGNETIC FI

[6]

Radler K.-H., 1974, ASTRON NACHR, V295, P265

[7]

ROBERTS PH, 1990, SUN COOL STARS ACTIV

[8]

RUDIGER G, 1988, DIFFERENTIAL ROTATIO

[9]

RUDIGER G, 1974, ASTRON NACHR, V295, P275

[10] CONVECTION IN ROTATING STARS [J].

TAYLER, RJ .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1973, 165 (01) :39-52

← 1 →