Dynamics of primordial black hole formation

J. C. Niemeyer and K. Jedamzik
Phys. Rev. D 59, 124013 – Published 18 May 1999
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Abstract

We present a numerical investigation of the gravitational collapse of horizon-size density fluctuations to primordial black holes (PBHs) during the radiation-dominated phase of the early Universe. The collapse dynamics of three different families of initial perturbation shapes, imposed at the time of horizon crossing, is computed. The perturbation threshold for black hole formation, needed for estimations of the cosmological PBH mass function, is found to be δc0.7 rather than the generally employed δc1/3 if δ is defined as ΔM/Mh, the relative excess mass within the initial horizon volume. In order to study the accretion onto the newly formed black holes, we use a numerical scheme that allows us to follow the evolution for long times after formation of the event horizon. In general, small black holes (compared to the horizon mass at the onset of the collapse) give rise to a fluid bounce that effectively shuts off accretion onto the black hole, while large ones do not. In both cases, the growth of the black hole mass owing to accretion is insignificant. Furthermore, the scaling of black hole mass with the distance from the formation threshold, known to occur in near-critical gravitational collapse, is demonstrated to apply to primordial black hole formation.

  • Received 5 June 1998

DOI:https://doi.org/10.1103/PhysRevD.59.124013

©1999 American Physical Society

Authors & Affiliations

J. C. Niemeyer

  • University of Chicago, Department of Astronomy and Astrophysics, 5640 South Ellis Avenue, Chicago, Illinois 60637

K. Jedamzik

  • Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching, Germany

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Issue

Vol. 59, Iss. 12 — 15 June 1999

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