A NEWTONIAN DESCRIPTION OF THE GEOMETRY AROUND A ROTATING BLACK-HOLE

被引：45

作者：

CHAKRABARTI, SK ^{[1
]}

KHANNA, R ^{[1
]}

机构：

[1] LANDESSTERNWARTE HEIDELBERG,W-6900 HEIDELBERG,GERMANY

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 1992年 / 256卷 / 02期

关键词：

ACCRETION; ACCRETION DISKS; BLACK HOLE PHYSICS; RELATIVITY;

D O I：

10.1093/mnras/256.2.300

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We suggest that most of the relevant properties of the Kerr space-time could be retrieved by suitably choosing a scalar potential which we present here. This potential can be used in the same manner as one uses the gravitational potential in Newtonian flat space-time. We present examples using both the general relativistic equations and our potential. The examples include test-particle motion and fluid motion around a Kerr black hole. as well as the evolution of the ellipticity of a self-gravitating, slowly rotating collapsing star.

引用

页码：300 / 306

页数：7

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