Computations of primordial black-hole formation

By I. Musco, J. Miller, Luciano Rezzolla. 2004

297 citations recorded by the source corpus.

Results are presented from general relativistic numerical computations of primordial black-hole formation during the radiation-dominated era of the universe. Growing-mode perturbations are specified within the linear regime and their subsequent evolution is followed as they become nonlinear. We use a spherically symmetric Lagrangian code and study both super-critical perturbations, which go on to produce black holes, and sub-critical perturbations, for which the overdensity eventually disperses into the background medium. For super-critical perturbations, we confirm the results of previous work concerning scaling laws but note that the threshold amplitude for a perturbation to lead to black-hole formation is substantially reduced when the initial conditions are taken to represent purely growing modes. For sub-critical cases, where an initial collapse is followed by a subsequent re-expansion, strong compressions and rarefactions are seen for perturbation amplitudes near to the threshold. We have also investigated the effect of including a significant component of vacuum energy and have calculated the resulting changes in the threshold and in the slope of the scaling law.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/224af145826e239242036461c983f77c5206070d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. B. Carr
2. Florian Kuhnel
3. Juan García-Bellido
4. C. Byrnes
5. K. Kohri
6. V. Vennin
7. T. Terada
8. S. Young

In Nuclear and High Energy Physics

1. B. Carr
2. Florian Kuhnel
3. Juan García-Bellido
4. C. Byrnes
5. K. Kohri
6. S. Young
7. T. Terada
8. I. Musco

Citations in the corpus

• Primordial black hole formation and abundance: contribution from the non-linear relation between the density and curvature perturbation (2019, methodology): “The threshold value for collapse is typically stated in terms of the volume-averaged density contrast (as for example in [29, 31]), which corresponds to a top-hat window function — suggesting a top-hat function should be used.”
• A Brief Review on Primordial Black Holes as Dark Matter (2021, background): “2, with cs 1/3 the sound speed at the radiation epoch (Carr, 1975) More refined results show that the PBH mass is given by a scaling relation with the overdensity δ, MPBH κ(δ − δc) (Niemeyer and Jedamzik, 1998; Niemeyer and Jedamzik, 1999), where κ and α are order unity constants, which depend on th”
• PRIMORDIAL BLACK HOLE FORMATION IN THE MATTER-DOMINATED PHASE OF THE UNIVERSE (2016, background): “The results of numerical relativity simulations in spherical symmetry give the threshold d 0.42 0.50c˜ – (Shibata & Sasaki 1999; Musco et al. 2005; Polnarev & Musco 2007; Musco et al. 2009; Musco & Miller 2013; Harada et al. 2015).”
• Primordial black holes and gravitational waves from parametric amplification of curvature perturbations (2019, background): “Gaussian distribution of perturbations 3 (M) ˆ PBH(M) ˆ tot = erfc 0 @q c 2˙2 M 1 A; (3.1) where ’0:2 is a correction factor [78], c’0:45 is the critical density contrast above which PBHs will form [79], 4 and ˙2 M = R 1 0 (dq=q)W~ 2(R= k 1 M ;q) 16 81 (q=k M) 4T2(= k M ;q)P R(q) is the variance of”
• Primordial Black Holes as Dark Matter: Recent Developments (2020, background): “[57] Ilia Musco, John Miller, and Luciano Rezzolla, “Computations of primordial black hole formation,” Classical Quantum Gravity 22, 1405–1424 (2005), arXiv:gr-qc/0412063 [gr-qc].”
• The exponential tail of inflationary fluctuations: consequences for primordial black holes (2019, methodology): “More realistic approaches incorporate the full realspace profile of the density contrast across the inhomogeneity, either numerically or by studying the compaction function [83–86].”