Highly eccentric inspirals into a black hole
arXiv:1511.01498 · doi:10.1103/PhysRevD.93.064024
Abstract
We model the inspiral of a compact stellar-mass object into a massive nonrotating black hole including all dissipative and conservative first-order-in-the-mass-ratio effects on the orbital motion. The techniques we develop allow inspirals with initial eccentricities as high as and initial separations as large as to be evolved through many thousands of orbits up to the onset of the plunge into the black hole. The inspiral is computed using an osculating elements scheme driven by a hybridized self-force model, which combines Lorenz-gauge self-force results with highly accurate flux data from a Regge-Wheeler-Zerilli code. The high accuracy of our hybrid self-force model allows the orbital phase of the inspirals to be tracked to within radians or better. The difference between self-force models and inspirals computed in the radiative approximation is quantified.
Updated to reflect published version
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