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Spin Diagrams for Equal-Mass Black-Hole Binaries with Aligned Spins

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arxiv 0708.3999 v2 pith:IQP3NDAJ submitted 2007-08-29 gr-qc astro-ph

Luciano Rezzolla , Ernst Nils Dorband , Christian Reisswig , Peter Diener , Denis Pollney , Erik Schnetter , Bela Szilagyi This is my paper · ORCID
classification gr-qcastro-ph
keywords spinsblack-holealignedbinaryspinsystemsangularblack
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Binary black-hole systems with spins aligned with the orbital angular momentum are of special interest as they may be the preferred end-state of the inspiral of generic supermassive binary black-hole systems. In view of this, we have computed the inspiral and merger of a large set of binary systems of equal-mass black holes with spins aligned with the orbital angular momentum but otherwise arbitrary. By least-square fitting the results of these simulations we have constructed two "spin diagrams" which provide straightforward information about the recoil velocity |v_kick| and the final black-hole spin a_fin in terms of the dimensionless spins a_1 and a_2 of the two initial black holes. Overall they suggest a maximum recoil velocity of |v_kick|=441.94 km/s, and minimum and maximum final spins a_fin=0.3471 and a_fin=0.9591, respectively.

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Cited by 2 Pith papers

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  1. A Possible Triple Formation Scenario of Binary Black Hole Merge With One In Pair-instability Supernova Mass Gap

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    An isolated hierarchical triple channel with chemically homogeneous evolution and triple common envelope can produce PISN mass-gap BBH mergers matching GW190706 at ~22% of the observed rate.

  2. Eccentricity Effects on Modeling Dynamic Quantities and Their Correlations in Binary Black Hole Mergers

    gr-qc 2025-01 conditional novelty 5.0 of 10

    Varying the initial orbital phase of an eccentric binary black hole at fixed eccentricity produces an envelope of radiated energy, momentum, and spin, so eccentric mergers span broad domains of remnant properties rela...

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