A Newtonian description of the geometry around a rotating black hole

Details A Newtonian description of the geometry around a rotating black hole A Newtonian description of the geometry around a rotating black hole

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..300c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 2, May 15, 1992, p. 300-306.

Astronomy and Astrophysics

Astronomy

24

Accretion Disks, Black Holes (Astronomy), Relativity, Space-Time Functions, Gravitational Collapse, Particle Motion

Scientific paper

It is suggested that most of the relevant properties of the Kerr space-time could be retrieved by suitably choosing a scalar potential presented here. This potential can be used in the same manner as one uses the gravitational potential in Newtonian flat space-time. Examples are presented using both the general relativistic equations an the proposed potential. The examples include test-particle motion and fluid motion around Kerr black hole as well as the evolution of the ellipticity of a self-gravitating slowly rotating collapsing star.

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