Eikonal quasinormal modes for accelerating black holes are determined by the angular velocity and Lyapunov exponent of null geodesics, yielding universal greybody factors for any spin and explicit shadow radii that reduce to the Reissner-Nordström case when acceleration vanishes.
Exploring black hole superkicks
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
abstract
Recent calculations of the recoil velocity in black-hole binary mergers have found kick velocities of $\approx2500 $km/s for equal-mass binaries with anti-aligned initial spins in the orbital plane. In general the dynamics of spinning black holes can be extremely complicated and are difficult to analyze and understand. In contrast, the ``superkick'' configuration is an example with a high degree of symmetry that also exhibits exciting physics. We exploit the simplicity of this ``test case'' to study more closely the role of spin in black-hole recoil and find that: the recoil is with good accuracy proportional to the difference between the $(l = 2, m = \pm 2)$ modes of $\Psi_4$, the major contribution to the recoil occurs within $30M$ before and after the merger, and that this is after the time at which a standard post-Newtonian treatment breaks down. We also discuss consequences of the $(l = 2, m = \pm 2)$ asymmetry in the gravitational wave signal for the angular dependence of the SNR and the mismatch of the gravitational wave signals corresponding to the north and south poles.
citation-role summary
background 3
citation-polarity summary
roles
background 3polarities
background 3representative citing papers
Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.
IMRPhenomXPHM is a new computationally efficient phenomenological model for precessing binary black hole gravitational-wave signals that incorporates higher-order modes via twisting-up maps from non-precessing waveforms.
citing papers explorer
-
Eikonal quasinormal modes, greybody factors and shadow of charged accelerating black holes
Eikonal quasinormal modes for accelerating black holes are determined by the angular velocity and Lyapunov exponent of null geodesics, yielding universal greybody factors for any spin and explicit shadow radii that reduce to the Reissner-Nordström case when acceleration vanishes.
-
Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA
Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.
-
Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes
IMRPhenomXPHM is a new computationally efficient phenomenological model for precessing binary black hole gravitational-wave signals that incorporates higher-order modes via twisting-up maps from non-precessing waveforms.
- Recoil kicks from binary black hole mergers in GWTC catalogs: implications for retention and hierarchical mergers