Coalescence remnant of spinning binary black holes

  title={Coalescence remnant of spinning binary black holes},
  author={John G. Baker and Manuela Campanelli and Carlos O. Lousto and Ryoji Takahashi},
  journal={Physical Review D},
We compute the gravitational radiation generated in the evolution of a family of close binary black hole configurations, using a combination of numerical and perturbative approximation methods. We evolve the binaries with spins s aligned or counteraligned with the orbital angular momentum from near the innermost stable circular orbit down to the final single rotating black hole. For the moderately spinning holes studied here the remnant Kerr black holes formed at the end of an inspiral process… 

Figures and Tables from this paper

Understanding the fate of merging supermassive black holes
Understanding the fate of merging supermassive black holes in galactic mergers, and the gravitational wave emission from this process, are important LISA science goals. To this end, we present
The numerical relativity breakthrough for binary black holes
The evolution of black-hole (BH) binaries in vacuum spacetimes constitutes the two-body problem in general relativity. The solution of this problem in the framework of the Einstein field equations is
Remnant masses, spins and recoils from the merger of generic black hole binaries
We obtain empirical formulae for the final remnant black hole mass, spin, and recoil velocity from merging black hole binaries (BHBs) with arbitrary mass ratios and spins. Our formulae are based on
Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries
We evolve equal-mass, equal-spin black-hole binaries with specific spins ofa=mH � 0:925, the highest spins simulated thus far and nearly the largest possible for Bowen-York black holes, in a set of
Spacelike gravitational radiation extraction from rotating binary black holes
We introduce an alternate method for gravitational radiation extraction for binary black hole mergers where we do not use a single extraction radius at the intermediate field region but instead use a
Massive Black Hole Binary Evolution
Coalescence of binary supermassive black holes (SBHs) would constitute the strongest sources of gravitational waves to be observed by LISA. While the formation of binary SBHs during galaxy mergers is
Black-hole binaries, gravitational waves, and numerical relativity
Understanding the predictions of general relativity for the dynamical interactions of two black holes has been a long-standing unsolved problem in theoretical physics. Black-hole mergers are
The RIT binary black hole simulations catalog
The RIT numerical relativity group is releasing a public catalog of black-hole-binary waveforms. The initial release of the catalog consists of 126 recent simulations that include precessing and
Properties and Astrophysical Implications of the 150 M⊙ Binary Black Hole Merger GW190521
The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85 − 14 + 21 M⊙ and 66 − 18 + 17 M⊙, compared
Further insight into gravitational recoil
We test the accuracy of our recently proposed empirical formula to model the recoil velocity imparted to the merger remnant of spinning, unequal-mass black-hole binaries. We study three families of