Quasilinear relaxation of the distribution function for collisionless, relativistic gravitating particles in an expanding universe

Details Quasilinear relaxation of the distribution function for collisionless, relativistic gravitating particles in an expanding universe Quasilinear relaxation of the distribution function for collisionless, relativistic gravitating particles in an expanding universe

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61..450v&link_type=abstract

(Astronomicheskii Zhurnal, vol. 61, May-June 1984, p. 450-459) Soviet Astronomy (ISSN 0038-5301), vol. 28, May-June 1984, p. 264

Astronomy and Astrophysics

Astronomy

Collisionless Plasmas, Distribution Functions, Gravitational Waves, Particle Diffusion, Relativistic Particles, Universe, Astronomical Models, Einstein Equations, Expansion, Perturbation Theory, Relaxation (Mechanics), Vlasov Equations

Scientific paper

In a model universe homogeneous and isotropic in the mean, potential-type and tensor-type perturbations of the spacetime metric and of the collisionless-particle (photons, neutrinos, ...) distribution function are considered. The Vlasov-Einstein equations yield expressions for the perturbation correlators. The influence of the potential and tensor fluctuations upon the rate of cosmological expansion and the collisionless-particle spectrum is treated in the random-phase approximation. For both types of perturbations the collisionless subsystem will undergo diffusion in momentum space, causing the particles to gain energy and strengthening the high-frequency part of their spectrum. The coupling of the cosmic background radiation with high-frequency gravitational waves has important astrophysical implications.

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