Development of voids in the thin-wall approximation

Details Development of voids in the thin-wall approximation Development of voids in the thin-wall approximation

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phdt........12p&link_type=abstract

Ph.D. Thesis Queens Univ., Kingston (Ontario). Dept. of Physics.

Astronomy and Astrophysics

Astrophysics

Background Radiation, Big Bang Cosmology, Galactic Clusters, Galactic Evolution, Spheres, Universe, Voids, Astrophysics, Cosmic Dust, Evolution (Development), Galactic Structure, Thin Walls

Scientific paper

The evolution of spherical voids in a Robertson-Walker background is studied within the context of the general relativistic thin-wall approximation. The background is taken to be a noninteracting mixture of dust and blackbody radiation. An extension of earlier work by Maeda and Sato with the refinements of background pressure, surface pressure, and interior mass is presented, with the void interior taken to be a vacuum. These refinements have important effects on the evolution of voids. The vacuum interior is replaced with an interior of Robertson-Walker radiation. The inclusion of radiation within the void has significant quantitative and important qualitative effects on void evolution. In general terms, the interior radiation pressure causes the voids to grow much more readily than vacuum voids. In particular, in a flat background, voids that do not collapse grow, at late times, like the particle horizon. Voids in an open background, on the other hand, tend to become comoving at late times. The formalism is applied to a replacement of the Robertson-Walker metric of the background with the de Sitter metric, retaining the Robertson-Walker interior. This permits examination of the simple inflationary scenario of a bubble of true vacuum expanding into a false vacuum background. It was found that, while the bubble grows, the growth is not as strong as might have been expected.

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