Cosmological Black Holes

Abstract

In this paper we propose a model for the formation of the cosmological voids. We show that cosmological voids can form directly after the collapse of extremely large wavelength perturbations into low-density black holes or cosmological black holes (CBH). Consequently the voids are formed by the comoving expansion of the matter that surrounds the collapsed perturbation. It follows that the universe evolves, in first approximation, according to the Einstein-Straus cosmological model. We discuss finally the possibility to detect the presence of these black holes through their weak and strong lensing effects and their influence on the cosmic background radiation.

14 pages, new completely revised version, to appear on GRG

References in corpus (4)

• Strong field limit of black hole gravitational lensing
• The Void Phenomenon
• Antibias in Clusters: The Dependence of M/L on Cluster Temperature
• Axially symmetric Einstein-Straus models

Cited by in corpus (13)

• Relativistic images of Schwarzschild black hole lensing
• Time delay and magnification centroid due to gravitational lensing by black holes and naked singularities
• Cosmological expansion and local physics
• Making sense of the bizarre behaviour of horizons in the McVittie spacetime
• Black Holes in the Universe: Generalized Lemaitre-Tolman-Bondi Solutions
• Porosity criterion for hyperbolic voids and the cosmic microwave background
• Strong gravitational lensing: why no central black holes?
• Cosmological Black Holes as Seeds of Voids in Galaxy Distribution
• Cosmological black holes as voids progenitors. I. Simulations
• Turnaround physics beyond spherical symmetry
• Black holes inside cosmic voids
• Singular shell embedded into a cosmological model
• The Cardy-Verlinde equation in a spherical symmetric gravitational collapse