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As shown by Teukolsky, the master equation governing the propagation of weakradiation in a black hole spacetime can be separated into four ordinarydifferential equations, one for each spacetime coordinate. (``Weak'' means theradiation's amplitude is small enough that its own gravitation may beneglected.) Unfortunately, it is difficult to accurately compute solutions tothe separated radial equation (the Teukolsky equation), particularly in anumerical implementation. The fundamental reason for this is that the Teukolskyequation's potentials are long ranged. For non-spinning black holes, one canget around this difficulty by applying transformations which relate theTeukolsky solution to solutions of the Regge-Wheeler equation, which has ashort-ranged potential. A particularly attractive generalization of thisapproach to spinning black holes for gravitational radiation (spin weight s =-2) was given by Sasaki and Nakamura. In this paper, I generalize Sasaki andNakamura's results to encompass radiation fields of arbitrary integer spinweight, and give results directly applicable to scalar (s = 0) andelectromagnetic (s = -1) radiation. These results may be of interest forstudies of astrophysical radiation processes near black holes, and of programsto compute radiation reaction forces in curved spacetime.Comment: 10 pages, no figures, to appear in Phys. Rev. D. Present version  updates the references, fixes some typos, and corrects some of the  Introductory tex

Computing radiation from Kerr black holes: Generalization of the Sasaki-Nakamura equation