Gravitational Radiation Reaction (original) (raw)

We give a short personally-biased review on the recent progress in our understanding of gravitational radiation reaction acting on a point particle orbiting a black hole. The main motivation of this study is to obtain sufficiently precise gravitational waveforms from inspiraling binary compact stars with a large mass ratio. For this purpose, various new concepts and techniques have been developed to compute the orbital evolution taking into account the gravitational self-force. Combining these ideas with a few supplementary new ideas, we try to outline a path to our goal here. * ) This subsection largely owes to discussion with N. Sago. * * ) When we reconstruct the metric perturbation from a solution of the master variable within the source distribution, more delicate treatment is necessary. 29) Below we use the assumption of the factorized form of the tensor Green function. This assumption is not necessary if we follow the derivation given by Wald, 28) and actually this assumption itself is not correct. 29) * ) We would like to come back to this point in future publication. * * ) There is another way given by Amos Ori during post-Capra discussion meeting (2003, Kyoto), which does not rely on the presence of GODS. We give a brief explanation of his argument here