2004/09/01 by R. Fujita, Ryuichi Fujita, H. Tagoshi +1 · 2 citations
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Pulsars and Gravitational Waves Research #Superconducting Materials and Applications #gr-qc
paper · pdf · doi:10.1143/ptp.112.415
published as Prog.Theor.Phys. 112 (2004) 415-450 · 36 pages,7 figures
crossref issued 2004/09/01 · crossref published 2004/09/01 · crossref published-print 2004/09/01 · openalex publication_date 2004/09/01 · arxiv created 2004/10/05 · crossref created 2005/02/28 · arxiv updated 2009/12/01 · crossref deposited 2019/01/31 · openalex created_date 2025/10/10 · crossref indexed 2026/07/30 · openalex updated_date 2026/07/30
We discuss a numerical method to compute the homogeneous solutions of the Teukolsky equation which is the basic equation of the black hole perturbation method. We use the formalism developed by Mano, Suzuki and Takasugi, in which the homogeneous solutions of the radial Teukolsky equation are expressed in terms of two kinds of series of special functions, and the formulas for the asymptotic amplitudes are derived explicitly.Although the application of this method was previously limited to the analytical evaluation of the homogeneous solutions, we find that it is also useful for numerical computation. We also find that so-called "renormalized angular momentum parameter", ν, can be found only in the limited region of ω for each l,m if we assume ν is real (here, ω is the angular frequency, and l and m are degree and order of the spin-weighted spheroidal harmonics respectively). We also compute the flux of the gravitational waves induced by a compact star in a circular orbit on the equatorial plane around a rotating black hole. We find that the relative error of the energy flux is about 10-14 which is much smaller than the one obtained by usual numerical integration methods.