Approximate Black Holes for Numerical Relativity

Abstract

Spherically symmetric solutions in Brans-Dicke theory of relativity with zero coupling constant, $\omega =0$, are derived in the Schwarzschild line-element. The solutions are obtained from a cubic transition equation with one small parameter. The exterior space-time of one family of solutions is arbitrarily close to the exterior Schwarzschild space-time. These nontopological solitons have some similarity with soliton stars, and are proposed as candidates for {\em approximate black holes} for the use in numerical relativity, in particular for treatment of horizon boundary conditions.

Postscript, 2 figures

References in corpus (3)

• Gravitational-Radiation Damping of Compact Binary Systems to Second Post-Newtonian order
• Gravitational waves from inspiralling compact binaries: Energy loss and waveform to second--post-Newtonian order
• "Are Black Holes in Brans-Dicke Theory precisely the same as in General Relativity?"

Cited by in corpus (7)

• Critical phenomena in gravitational collapse
• Conformal Thin-Sandwich Solver for Generic Initial Data
• Numerical Integration of Nonlinear Wave Equations for General Relativity
• Instability of an "Approximate Black Hole"
• Cosmon Lumps and Horizonless Black Holes
• Shadows of naked singularity in Brans-Dicke gravity
• Unveiling horizons in quantum critical collapse