Curvature profiles as initial conditions for primordial black hole formation

By A. Polnarev, I. Musco. 2006

142 citations recorded by the source corpus.

This work is part of an ongoing research programme to study possible primordial black hole (PBH) formation during the radiation-dominated era of the early universe. Working within spherical symmetry, we specify an initial configuration in terms of a curvature profile, which represents initial conditions for the large amplitude metric perturbations, away from the homogeneous Friedmann–Robertson–Walker model, which are required for PBH formation. Using an asymptotic quasi-homogeneous solution, we relate the curvature profile with the density and velocity fields, which at an early enough time, when the length scale of the configuration is much larger than the cosmological horizon, can be treated as small perturbations of the background values. We present general analytic solutions for the density and velocity profiles. These solutions enable us to consider in a self-consistent way the formation of PBHs in a wide variety of cosmological situations with the cosmological fluid being treated as an arbitrary mixture of different components with different equations of state. We obtain the analytical solutions for the density and velocity profiles as functions of the initial time. We then use two different parametrizations for the curvature profile and follow numerically the evolution of initial configurations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2154d37671b38491f81e62b3340bbf0bd8dfc0e5

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In Astronomy and Astrophysics

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

In Nuclear and High Energy Physics

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

Citations in the corpus

• 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 hole formation and abundance: contribution from the non-linear relation between the density and curvature perturbation (2019, background): “Since then, there has been extensive work to determine the collapse threshold [17, 20, 25, 27–31], as well as discussions about the appropriate parameter to use to determine whether a perturbation will collapse”
• Threshold for primordial black holes: Dependence on the shape of the cosmological perturbations (2018, methodology): “To do this I will follow the approach used in Polnarev & Musco (2007) [16], where supra horizon initial perturbations are described in terms of the non linear curvature profile, used to specify initial conditions for numerical simulations analogous to the ones performed in [12], using an asymptotic…”
• Solar-mass primordial black holes explain NANOGrav hint of gravitational waves (2020, background): “where we have assumed that the primordial curvature perturbations have the Gaussian statistics, δc is the critical value of the coarse-grained density perturbations that produces a PBH [58–64], for which we take δc = 0.”
• 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].”