Critical phenomena at the threshold of immediate merger in binary black hole systems: the extreme mass ratio case

Abstract

In numerical simulations of black hole binaries, Pretorius and Khurana [Class. Quant. Grav. {\bf 24}, S83 (2007)] have observed critical behaviour at the threshold between scattering and immediate merger. The number of orbits scales as $n\simeq -\gamma \ln |p-p_{\ast }|$ along any one-parameter family of initial data such that the threshold is at $p=p_{\ast }$. Hence they conjecture that in ultrarelavistic collisions almost all the kinetic energy can be converted into gravitational waves if the impact parameter is fine-tuned to the threshold. As a toy model for the binary, they consider the geodesic motion of a test particle in a Kerr black hole spacetime, where the unstable circular geodesics play the role of critical solutions, and calculate the critical exponent $\gamma$. Here, we incorporate radiation reaction into this model using the self-force approximation. The critical solution now evolves adiabatically along a sequence of unstable circular geodesic orbits under the effect of the self-force. We confirm that almost all the initial energy and angular momentum are radiated on the critical solution. Our calculation suggests that, even for infinite initial energy, this happens over a finite number of orbits given by $n_{\infty }\simeq 0.41/\eta$, where $\eta$ is the (small) mass ratio. We derive expressions for the time spent on the critical solution, number of orbits and radiated energy as functions of the initial energy and impact parameter.

Version published in PRD

References in corpus (4)

• Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion
• Black Hole Mergers and Unstable Circular Orbits
• Cross section, final spin and zoom-whirl behavior in high-energy black hole collisions
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