Binary Black Hole Mergers: Spin and Mass Ratio Effects on Gravitational Waveforms

Abstract

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. Weinvestigatetheinfluenceoftheseparametersonremnantproperties,includingthefinalspin(𝜒𝑓),fractionalmass loss (𝑀FL), and peak gravitational-wave strain (ℎmax). By systematically analysing the trends across four distinct spin alignments (PP, PN, BP, BN), we identify non-monotonic behaviours 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 from 2% to 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.

Keywords

• Binary black holes
• gravitational waves
• high energy astrophysical phenomena
• numerical relativity
• remnant black holes

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