Abstract
To accurately obtain the waveform template of gravitational waves,substantial computational resources and extremely high pre-cision are often required.In a previous study,we employed the confluent Heun function to obtain an exact solution to the Teukolsky equation.This approach allowed us to efficiently and accurately calculate the gravitational wave flux for a particle in circular orbits around a Schwarzschild black hole.Building on this method,we now extend its application to calculate the asymptotic gravitational wave fluxes from a particle in generic orbits around a near-extreme Kerr black hole.Our extended method proves particularly effective in handling computational challenges associated with large eccentricities(e=0.9),higher spins(a=0.999),higher harmonic modes,and strong-field regions.The results we obtained significantly outperform those derived from the numerical integration method based on the Mano-Suzuki-Takasugi method.
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