Scalar Gravitational Waves and Observational Limitations for the EnergyMomentum Tensor of a Gravitational Field
Abstract
From the point of view of a totally nonmetric model of the theory of gravitational interaction, i.e., in the bounds of a consistent dynamic description of gravitation (gravidynamics) a possibility is pointed out of additional loss of energy for the radiation of scalar gravitational waves. Such a radiation arises due to (in particular, periodic) variations, for example, sphericallysymmetric pulsations, in a radiating system and is connected with time change of kinetic energy of system. The scalar gravitational ‘luminosity’ in gravidynamics is of the same order (∼G/c ^{5}) as the system energy loss for the radiation of ‘usual’ tensor gravitational waves of general relativity. Perhaps, for a binary system with a nonzero eccentricity it is necessary to account for the influence of scalar radiation on a secular variation of the companion's orbit parameters. The contribution of the scalar radiation into a total gravitational ‘luminosity’ of the system with a radio pulsar PSR 1913+16 can be of the value about 2.2% of the radiation power of the tensor gravitational waves. It can have a considerable effect at measurements of the fall rate of orbital period (P _{ b }) of the binary system, and the corresponding contribution intoP _{ b } can be equal to ∆P _{ b }≈0.053x10^{12} ss^{1}.
 Publication:

Astrophysics and Space Science
 Pub Date:
 December 1992
 DOI:
 10.1007/BF00644299
 Bibcode:
 1992Ap&SS.198...53S
 Keywords:

 Binary Stars;
 Gravitational Fields;
 Gravitational Waves;
 Pulsars;
 Radio Stars;
 Computational Astrophysics;
 Eccentricity;
 Luminosity;
 Orbital Mechanics;
 Relativity;
 Astrophysics