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Journal Article

A no-hair test for binary black holes


Ghosh,  Abhirup
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Dhanpal, S., Ghosh, A., Mehta, A. K., Ajith, P., & Sathyaprakash, B. S. (2019). A no-hair test for binary black holes. Physical Review D, 99: 104056. doi:10.1103/PhysRevD.99.104056.

Cite as: http://hdl.handle.net/21.11116/0000-0003-BFF6-1
One of the consequences of the black-hole "no-hair" theorem in general relativity (GR) is that gravitational radiation (quasi-normal modes) from a perturbed Kerr black hole is uniquely determined by its mass and spin. Thus, the spectrum of quasi-normal mode frequencies have to be all consistent with the same value of the mass and spin. Similarly, the gravitational radiation from a coalescing binary black hole system is uniquely determined by a small number of parameters (masses and spins of the black holes and orbital parameters). Thus, consistency between different spherical harmonic modes of the radiation is a powerful test that the observed system is a binary black hole predicted by GR. We formulate such a test, develop a Bayesian implementation, demonstrate its performance on simulated data and investigate the possibility of performing such a test using previous and upcoming gravitational wave observations.