Gravitational radiation and spiralling time of close binary systems (IV)

Abstract

Binary systems with their primary and secondary component masses less than 2M☉ have been investigated to evaluate the rate of emission of gravitational energy (Pв) and spiralling time (τₒ) for them. In all twenty-two binary systems have been considered. It is found that in spite of the same mass range, these systems form two distinct groups. New relations have been given between Pв and τₒ for each group. For a few eccentric orbit systems the rate of decay of orbital periods due to loss of energy from the systems via gravitational radiation emission has also been given and compared with a short-period binary pulsar.