2023/04/19 by İsmail Özbakır, Özbakır, İsmail, K. Yakut +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #Magnetic confinement fusion research #Pulsars and Gravitational Waves Research #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.2304.09396
openalex publication_date 2023/04/19 · openalex created_date 2023/04/22 · openalex updated_date 2026/08/02
We present a comprehensive parameter-space study of binary black hole (BBH) mergers using the SEOBNRv4_opt waveform model. Our analysis spans ∼ 106 simulated waveforms across a broad range of mass ratios \( q = (m1)/(m2) ∈ [1.0, 2.0] \) and aligned spin configurations. We investigate the influence of these parameters on remnant properties, including final spin (χf), fractional mass loss (MFL), and peak gravitational-wave strain (hmax). By systematically analyzing the trends across four distinct spin alignments (PP, PN, BP, BN), we identify non-monotonic behaviors and turning points in MFL and χf as functions of q, highlighting subtle dynamical effects that are not explicitly emphasized in commonly used remnant fitting formulae. While confirming known correlations from numerical relativity, our results offer new insights into parameter interactions and waveform morphology, with implications for BBH population studies and remnant characterization. Across all configurations studied, the fractional mass loss due to gravitational-wave emission ranges between 2% and 9.5%, depending on the mass ratio and spin alignment. This work may also aid in understanding the spin and mass distributions of the more massive black holes formed post-merger, thereby contributing to future remnant-based astrophysical inference.