Relativistic Astrophysics with Resonant Multiple Inspirals

Abstract

We show that a massive black hole binary might resonantly trap a small third body (e.g. a neutron star) down to a stage when the binary becomes relativistic due to its orbital decay by gravitational radiation. The final fate of the third body would be quite interesting for relativistic astrophysics. For example, the parent binary could expel the third body with a velocity more than 10% of the speed of light. We also discuss the implications of this three-body system for direct gravitational wave observation.

6 pages, 4 figures, Phys.Rev.D in press

References in corpus (4)

• Getting a kick out of numerical relativity
• Three-body equations of motion in successive post-Newtonian approximations
• Gravitational wave forms for a three-body system in Lagrange's orbit: parameter determinations and a binary source test
• Resonance Trapping in Protoplanetary Disks. I. Coplanar Systems

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