Pith. sign in

REVIEW 3 cited by

Alignment of the spins of supermassive black holes prior to coalescence

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv astro-ph/0703054 v2 pith:DMUY6DJW submitted 2007-03-05 astro-ph gr-qc

Tamara Bogdanovic , Christopher S. Reynolds , M. Coleman Miller (University of Maryland) This is my paper · ORCID
classification astro-phgr-qc
keywords blackgalacticalignmentcoalescenceescapegalaxiesholeholes
verification ladder T0 review T1 audit T2 compute T3 formal
0 comments
read the original abstract

Recent numerical relativistic simulations of black hole coalescence suggest that in certain alignments the emission of gravitational radiation can produce a kick of several thousand kilometers per second. This exceeds galactic escape speeds, hence unless there a mechanism to prevent this, one would expect many galaxies that had merged to be without a central black hole. Here we show that in most galactic mergers, torques from accreting gas suffice to align the orbit and spins of both black holes with the large-scale gas flow. Such a configuration has a maximum kick speed <200 km/s, safely below galactic escape speeds. We predict, however, that in mergers of galaxies without much gas, the remnant will be kicked out several percent of the time. We also discuss other predictions of our scenario, including implications for jet alignment angles and X-type radio sources.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Relativistic gas accretion onto supermassive black Hole binaries from inspiral through merger

    astro-ph.HE 2025-02 conditional novelty 7.0 of 10

    A new code hand-off enables a 3D GRMHD simulation of an equal-mass nonspinning supermassive black hole binary from 20M separation through merger and postmerger, showing minidisk dissolution, declining accretion, and a...

  2. The Bardeen-Petterson effect in accreting supermassive black-hole binaries: disc breaking and critical obliquity

    astro-ph.HE 2021-11 unverdicted novelty 7.0 of 10

    3D simulations recover the critical obliquity for disc breaking predicted by semi-analytic models and reveal additional stabilization by spiral arms that can prevent breaking.

  3. Improved post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries

    gr-qc 2025-02 conditional novelty 6.0 of 10

    The paper presents pyEFPE, a validated and publicly available frequency-domain post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries, with up to about a fifteen-fold speedup.

Pith tools