2025/08/28 by Cáceres-Barbosa, Viviana A.
#FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc)
paper · doi:10.48550/arxiv.2508.21216
We analyze the spherical harmonic mode amplitudes of quasi-circular, nonprecessing binary black hole mergers using 283 numerical relativity (NR) simulations from the SXS, RIT, and MAYA catalogs. We construct fits using the leading-order post-Newtonian (PN) dependence on intrinsic parameters, replacing the PN velocity with fit coefficients. We compare these to polynomial fits in symmetric mass ratio and spin. We analyze (ℓ, m) modes with ℓ ≤ 4 from late inspiral (t = -500M relative to the (2,2) peak) to post-merger (t = 40M). For nonspinning systems, the (2,2), (2,1), and (3,3) modes retain the leading-order PN dependence on mass ratio throughout the merger. Higher-order modes deviate from the PN dependence only near and after the merger, where polynomial fits of degree N ≤ 3 can capture the amplitude behavior up to 40M. For aligned-spin systems at fixed mass ratio, the (2,1) mode retains its PN spin dependence, while the (3,2) and (4,3) modes exhibit a quadratic spin dependence near merger. The PN-inspired fits lose accuracy with increasing mass ratio, particularly near merger. Results broadly agree across catalogs, though discrepancies appear in the (3,1), (4,2), and (4,1) modes, likely from resolution differences. Our results clarify the extent to which PN structure persists in mode amplitudes and show that simple polynomial models can capture strong-field behavior near merger, enabling efficient and interpretable waveform modeling in this regime.