Primordial black hole formation from a nonspherical density profile with a misaligned deformation tensor
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arXiv
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| Format: | Preprint |
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2024
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| author | Yoo, Chul-Moon |
| author_facet | Yoo, Chul-Moon |
| contents | We perform the numerical simulation of primordial black hole formation from a nonspherical profile of the initial curvature perturbation $ζ$. We consider the background expanding universe filled with the perfect fluid with the linear equation of state $p=wρ$ ($w=1/3$ or $1/5$), where $p$ and $ρ$ are the pressure and the energy density, respectively. The initial condition is set in a way such that the principal directions of the second derivatives of $ζ$ and $\triangle ζ$ at the central peak are misaligned, where $\triangle$ is the Laplacian. In this setting, since the linearized density is proportional to $\triangle ζ$, the inertia tensor and deformation tensor $\partial_i\partial_j ζ$ are misaligned. Thus tidal torque may act and the spin of a resultant primordial black hole would be non-zero in general, although it is estimated to be very small from previous perturbative analyses. As a result, we do not find a finite value of the spin within our numerical precision, giving support for the negligibly small value of the black hole spin for $1/5\lesssim w \lesssim 1/3$. More specifically, our results suggest that the dimensionless PBH spin $s$ is typically so small that $s\ll0.1$ for $w\gtrsim0.2$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_11147 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Primordial black hole formation from a nonspherical density profile with a misaligned deformation tensor Yoo, Chul-Moon General Relativity and Quantum Cosmology Cosmology and Nongalactic Astrophysics High Energy Physics - Theory We perform the numerical simulation of primordial black hole formation from a nonspherical profile of the initial curvature perturbation $ζ$. We consider the background expanding universe filled with the perfect fluid with the linear equation of state $p=wρ$ ($w=1/3$ or $1/5$), where $p$ and $ρ$ are the pressure and the energy density, respectively. The initial condition is set in a way such that the principal directions of the second derivatives of $ζ$ and $\triangle ζ$ at the central peak are misaligned, where $\triangle$ is the Laplacian. In this setting, since the linearized density is proportional to $\triangle ζ$, the inertia tensor and deformation tensor $\partial_i\partial_j ζ$ are misaligned. Thus tidal torque may act and the spin of a resultant primordial black hole would be non-zero in general, although it is estimated to be very small from previous perturbative analyses. As a result, we do not find a finite value of the spin within our numerical precision, giving support for the negligibly small value of the black hole spin for $1/5\lesssim w \lesssim 1/3$. More specifically, our results suggest that the dimensionless PBH spin $s$ is typically so small that $s\ll0.1$ for $w\gtrsim0.2$. |
| title | Primordial black hole formation from a nonspherical density profile with a misaligned deformation tensor |
| topic | General Relativity and Quantum Cosmology Cosmology and Nongalactic Astrophysics High Energy Physics - Theory |
| url | https://arxiv.org/abs/2403.11147 |