Primordial black hole formation with full numerical relativity

Abstract

We study the formation of black holes from subhorizon and superhorizon perturbations in a matter dominated universe with 3+1D numerical relativity simulations. We find that there are two primary mechanisms of formation depending on the initial perturbation's mass and geometry -- via $\text{direct collapse}$ of the initial overdensity and via $\text{post-collapse accretion}$ of the ambient dark matter. In particular, for the latter case, the initial perturbation does not have to satisfy the hoop conjecture for a black hole to form. In both cases, the duration of the formation the process is around a Hubble time, and the initial mass of the black hole is $M_{\mathrm{BH}}\sim 10^{-2}{H}^{-1}{M}_{\mathrm{Pl}}^2$. Post formation, we find that the PBH undergoes rapid mass growth beyond the self-similar limit $M_{\mathrm{BH}}\propto H^{-1}$, at least initially. We argue that this implies that most of the final mass of the PBH is accreted from its ambient surroundings post formation.

arXiv comment12 pages, 8 figures. 2 YouTube videos here: https://youtube.com/playlist?list=PLSkfizpQDrcZuKZPQydJA9l_pxxWpqIMz

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