Gravitational Radiation Energy Research Articles

Gravitational radiation from a binary system

It is shown that the gravitational radiation energy flux from a quasiperiodic binary system is given by the quadrupole formula contribution plus a nonlinear contribution which has been neglected in the past. The latter is found to depend on both the intensity of the gravitational field and the history of the radiating system. For PSR 1913+16, the nonlinear contribution to the energy flux may be neglected relative to that of the quadrupole formula.

Is collapse of a deformed star always effectual for gravitational radiation?

We have computed the energy of gravitational radiation from an axially symmetric, non-rotating dust shell of mass m falling into a Schwarzschild black hole of mass M ⪢ m. Both prolate and oblate dust shells are examined. A strongly deformed dust shell radiates less gravitational waves than a moderately deformed one. The radiation energy from a dust shell is less than that from a test particle, which is contrary to the newtonian result of Thuan and Ostriker which did not take phase cancellation effects into account.

Gravitational radiation energy loss in scattering problems and the Einstein quadrupole formula

The equations of motion necessary to compute the emission of gravitational radiation during small-angle scattering according to general relativity using a fast approximation method are presented. In addition a generalization of the Lagrange expansion method to convert Poincaré invariant equations to newtonian ones is given.

The approximation of radiative effects in relativistic gravity - Gravitational radiation reaction and energy loss in nearly Newtonian systems

An argument is presented to determine the accuracy with which a solution of Einstein's field equations of gravitation must be approximated in order to describe the dominant effects of gravitational radiation emission from weak-field systems. Several previous calculations are compared in the light of this argument, and some apparent discrepancies among them are resolved. The majority of these calculations support the 'quadrupole formulae' for gravitational radiation energy loss and radiation reaction.

Gravitational Radiation Quadrupole Formula is Valid for Gravitationally Interacting Systems

An argument is presented for the validity of the quadrupole formula for gravitational radiation energy loss in the far field of nearly Newtonian (e.g., binary stellar) systems. This argument differs from earlier ones in that it determines beforehand the formal accuracy of approximation required to describe gravitationally self-interacting systems, uses the corresponding approximate equation of motion explicitly, and evaluates the appropriate asymptotic quantities by matching along the correct space-time light cones.

Gravitational Radiation Energy Loss in Scattering Problems and the Einstein Quadrupole Formula.

Gravitational Radiation Energy Loss in Scattering Problems and the Einstein Quadrupole Formula.

Gravitational Radiation Energy Loss in Scattering Problems and the Einstein Quadrupole Formula

The energy loss due to the emission of gravitational radiation during small-angle scattering according to general relativity is computed by means of a fast approximation method. The results differs by a factor of about 2.3 from the one based on the assumption that the Einstein quadrupole formula applies to energy changes in the material source.

Gravitational Radiation from a Particle Falling Radially into a Schwarzschild Black Hole

We have computed the spectrum and energy of gravitational radiation from a point test particle of mass $m$ falling radially into a Schwarzschild black hole of mass $M\ensuremath{\gg}m$. The total energy radiated is about $0.0104m{c}^{2}(\frac{m}{M})$, 4 to 6 times larger than previous estimates; the energy is distributed among multipoles according to the empirical law ${E}_{2l\ensuremath{-}\mathrm{p}\mathrm{o}\mathrm{l}\mathrm{e}}\ensuremath{\approx}(\frac{0.44{m}^{2}{c}^{2}}{M}){e}^{\ensuremath{-}2l}$; and the total spectrum peaks at an angular frequency $\ensuremath{\omega}=\frac{0.32{c}^{3}}{\mathrm{GM}}$.