- General Relativity and Spacetime
- Einsteins field equations and Black Holes
- Kerr's rotating Black Holes
- Conclusion
- References
- About this document ...

**June 1996**

In this paper I will investigate the geometry around Black Holes, and how this affects freely falling relativistic particles along geodesics which is certainly not straight lines as in normal flat spacetime.
Stellar Black Holes are the relicts of collapsed massive stars which provides extreme mass-/energydensities. Nothing can escape from the Black Hole, not even light. This is because of the extreme curvature of space. The detailed description of Black Holes is included
in The Einstein Field Equations. Historically one of the first exact solutions to these equations was that of
Schwarzschild 1916 describing a spherical symmetric point mass, later identified as a Black Hole.

I will concentrate on the Schwarzschild-solution, describing a non-rotating Black Hole and the Kerr solution, describing Black Holes with
angular momentum. There exists of course more general - and complicated - solutions including charge, and
electromagnetic fields around the Black Holes. But I will not go into this exciting area.

The aim of this work is to use some of the fundamental results to get a view of the geometry around a Black Hole. Curvature is one of the most remarkable geometrical properties, but some other basic concepts has to be introduced, these are: world lines, geodesics and metric tensors.
Through out this text, I will use the space-like sign convention: (-,+,+,+) for the metrics considered; indices going from 1 to 3 are written in *latin* (i,k,..) denoting 3 space dimensions while indices going from 0 to 3 are written in *greek* ( ,..) denoting one time coordinate and 3 space coordinates.

Fri Jun 14 12:07:09 MDT 1996