The standard approach to initial data for both analytic and numerical computations of black hole collisions has been to use conformally flat initial geometries. This approach allows the simple superposition of holes with arbitrary mass, location and spin, but it is not suitable to the astrophysically relevant study of Kerr black holes. However, a nonconformally flat form of the 3-geometry can be chosen which allows fairly simple superposition of Kerr holes with arbitrary mass and spin. We present numerical initial data solutions representing rotating holes close enough, so that outside a common horizon the spacetime geometry is a perturbation of a single Kerr hole. Expressing these solutions in terms of the Weyl scalar psi_4, we are able to explore the dynamics by the numerical evolution of the Teukolsky equation.
19th Texas Symposium on Relativistic Astrophysics and Cosmology
- Pub Date:
- December 1998