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Session 13 - Gravitational Effects.
Display session, Monday, June 10
A calculation of the gravitational radiation emitted by a binary system (e.g., neutron stars, black holes) involves solving numerically extremely complicated non-linear equations. A zeroth order approximation scheme has recently been developed based upon a conformally flat description (CFM) of the spatial part of the metric tensor. This assumption essentially neglects energy loss due to gravitational radiation. This is a good approach in cases where the radiation damping is so small that the system can be considered to be in a quasi-stable orbit. But the inclusion of the gravitational radiation energy loss becomes essential during the inspiral prior to coalescence. We describe here a method to incorporate the gravitational radiation into the CFM scheme by adding a perturbation term to the conformally flat metric tensor to account for the essentially non-diagonal character of the metric of the gravitational waves. The dynamical equations are solved to first order in the perturbation complementing the soluti on obtained from the CFM scheme.
Program listing for Monday