Boyer-Lindquist coordinates

A generalization of the coordinates used for the metric of a Schwarzschild black hole that can be used to express the metric of a Kerr black hole.

The coordinate transformation from Boyer-Lindquist coordinates r, $heta$, $phi$ to cartesian coordinates x, y, z is given by:$\{x\}\; =\; sqrt\; \{r^2\; +\; a^2\}\; sin\; hetacosphi$:$\{y\}\; =\; sqrt\; \{r^2\; +\; a^2\}\; sin\; hetasinphi$:$\{z\}\; =\; r\; cos\; heta\; quad$

For a physical interpretation of the parameter "a", see the Kerr Metric.

References

*Boyer, R. H. and Lindquist, R. W. "Maximal Analytic Extension of the Kerr Metric". J. Math. Phys. 8, 265-281, 1967.
*Shapiro, S. L. and Teukolsky, S. A. "Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects". New York: Wiley, p. 357, 1983.