Calculating the Gravitational Self-Force in Schwarzschild Spacetime

2001/11/30 by Leor Barack, Yasushi Mino, Hiroyuki Nakano +2 · 8 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Experimental and Theoretical Physics Studies #Pulsars and Gravitational Waves Research #gr-qc

paper · pdf · doi:10.1103/physrevlett.88.091101

published as Phys.Rev.Lett.88:091101,2002 · Final publication version. Note corrections to Eqs. (13-15)

arxiv created 2002/02/14 · openalex publication_date 2002/02/19 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01

Abstract

We present a practical method for calculating the local gravitational self-force (often called "radiation-reaction force") for a pointlike particle orbiting a Schwarzschild black hole. This is an implementation of the method of mode-sum regularization, in which one first calculates the (finite) contribution to the force due to each individual multipole mode of the perturbation, and then applies a certain regularization procedure to the mode sum. Here we give the values of all the "regularization parameters" required for implementing this regularization procedure, for any geodesic orbit in Schwarzschild spacetime.

Citations

• Stability of a Schwarzschild Singularity

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• Two approaches for the gravitational self-force in black hole spacetime: Comparison of numerical results
• Discontinuous Galerkin method for computing gravitational waveforms from extreme mass ratio binaries
• Finite element computation of the gravitational radiation emitted by a pointlike object orbiting a nonrotating black hole
• Self-force viam-mode regularization and2+1Devolution: Foundations and a scalar-field implementation on Schwarzschild spacetime
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