Primordial Black Hole from Tensor-induced Density Fluctuation: First-order Phase Transitions and Domain Walls

TL;DR

This paper proposes a gauge-invariant mechanism for primordial black hole formation during first-order phase transitions and domain wall annihilation, linking cosmological observations with particle physics parameters.

Contribution

It introduces a novel, minimal, and model-independent tensor perturbation-based PBH formation mechanism, providing constraints on phase transition and domain wall parameters from existing data.

Findings

Asteroid mass PBHs can account for all dark matter within specific temperature ranges.

Predicted gravitational wave signals are within the detection capabilities of LISA and SKA.

Provides semi-analytical formulas connecting PBH properties with phase transition parameters.

Abstract

We present a novel \textit{gauge-invariant and minimal} formation mechanism of primordial black holes (PBHs) in first-order phase transition (FOPT) and domain walls (DW) separately. This is based on the first-order tensor perturbations, generated during FOPT from bubble collisions \& sound waves, and from DW annihilation, sourcing curvature, at second-order in perturbation theory. We show that the PBH formation implies \textit{model-independent constraints} on FOPT parameters ($\beta/H, \alpha, T_{\star}$ ) and on DW parameters, ($\alpha_{\rm ann}, V_{\rm bias}, \sigma$), from existing PBH constraints. We find that asteroid mass PBHs can become the entire dark matter (DM) of the Universe, for $T_{\star} \in (4 \times 10^{2}, 10^{4})$ GeV, for $\beta/H \simeq 6$, involving $\alpha >\mathcal{O}(1)$ values. The corresponding FOPT Gravitational Waves (GW) amplitude will have its characteristic peak at $\Omega_{\rm GW}^{\rm p} h^2$ $\sim \mathcal{O}(10^{-8})$ between frequencies $f_{\rm p} \in ({10^{-5},10^{-2}})$ Hz which is within the reach in LISA and SKA detectors. PBH as entire DM is possible for $\sigma^{1/3} \in [10^{6}, 10^{8}]$ TeV, for $V_{\rm bias}^{1/4} \in [10^7, 10^{10}]$ MeV with the corresponding GW amplitude peak from DW annihilation $\Omega_{\rm GW}^{\rm p} h^2$ $\sim \mathcal{O}(10^{-9})$ (for $\alpha_{\rm ann} \sim 10^{-2}$) and peak frequencies between $f_{\rm p} \in (4 \times {10^{-4},10^{-1}})$ Hz with ($T_{\rm ann} \in 4.5 \times [10^3, 10^6] $) GeV within the reach in LISA and ET detectors. We also provide semi-analytical formulae for the tensor-induced density spectrum, $P_{\delta^{(2)}}$, $M_{\rm PBH}$ and $f_{\rm PBH}$, relating them in terms of FOPT and DW parameters which in turn, are related to viable particle physics origin of such FOPT and DW, and therefore, constrain such microphysics, either in the visible, or in dark sector models.