Computational Modeling of Kerr Black Hole Ringdown Oscillations

Abstract

Our project investigates how the physical features of a Kerr black hole influence gravitational-wave ringdown oscillations after a binary black hole merger. Using a computational model based on quasi-normal mode approximations, the model generates inspiral, merger, and ringdown waveforms while allowing the final black hole's mass, dimensionless spin, mode composition, and detector noise level to be adjusted.The simulation also used frequency-domain analysis, including a power spectrum, to identify dominant ringdown frequencies.The results showed that increasing final black hole mass lowered the quasi-normal mode frequency and stretched the waveform over a longer timescale, while increasing spin produced more sustained oscillations with longer damping behavior times. The model also showed that detector noise distorted the waveform but did not fully remove the main ringdown structure. These findings support the hypothesis that Kerr black hole properties leave measurable signatures in gravitational-wave ringdown signals. Although the simulation is simplified and does not replace full numerical relativity or real detector analysis, it shows how computational modeling can connect general relativity, signal processing, and observable gravitational-wave behavior.This project provides a visual way to explore how black hole mass and spin can be inferred from post-merger oscillations.