Gravitational waves from quasi-spherical black holes

Abstract

A quasi-spherical approximation scheme, intended to apply to coalescing black holes, allows the waveforms of gravitational radiation to be computed by integrating ordinary differential equations.

4 revtex pages, 2 eps figures

References in corpus (5)

• Computing the merger of black-hole binaries: the IBBH problem
• Quasi-Spherical Light Cones of the Kerr Geometry
• Quasi-local first law of black-hole dynamics
• The close limit of colliding black holes: an update
• The characteristic treatment of black holes

Cited by in corpus (9)

• Black hole boundaries
• Marginally trapped tubes and dynamical horizons
• Isolated, slowly evolving, and dynamical trapping horizons: geometry and mechanics from surface deformations
• Energy and entropy conservation for dynamical black holes
• Energy conservation for dynamical black holes
• Angular momentum conservation for dynamical black holes
• Gravitational-wave dynamics and black-hole dynamics: second quasi-spherical approximation
• Quasi-spherical approximation for rotating black holes
• Energy of gravitational radiation in plane-symmetric space-times