Winds from fast rotating stars

被引：4

作者：

Bogovalov, S., V ^{[1
]}

Petrov, M. A. ^{[1
]}

Timofeev, V. A. ^{[1
]}

机构：

[1] Natl Res Nucl Univ MEPHI, Kashirskoje Shosse 31, Moscow 115409, Russia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 502卷 / 02期

关键词：

hydrodynamics; stars:; emission-line; Be; stars: mass-loss; winds; outflows; PSR B1259-63; STELLAR WINDS; GAMMA-RAYS; X-RAY; DISKS; EMISSION; PERIASTRON; SIMULATIONS; INSTABILITY; EVOLUTION;

D O I：

10.1093/mnras/stab036

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Numerical modelling of an isothermal wind from a fast rotating star is performed. Excitation of hydrodynamical turbulence and deviation of the shape of the stellar surface from a sphere are taken into account. Rotation and turbulence result in a dramatic increase of the mass flow rate from the star in comparison with a non-rotating one. The outflow occurs predominantly from a region on the stellar surface located at the equator. This flow expands rapidly due to thermal pressure. However, a disc-like flow at the equator is formed. The flow is more complicated near the pole. At large distances from the star a radially expanding wind is formed while close to the star some fraction of the outflow from the equatorial region falls down on to the stellar surface, producing a huge vortex. The dependence of the mass loss rate on the parameters of the star is presented.

引用

页码：2409 / 2418

页数：10

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