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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
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TY - JOUR
T1 - Primordial Black Hole Compaction Function from Stochastic Fluctuations in Ultraslow-Roll Inflation
AU - Raatikainen, Sami
AU - Räsänen, Syksy
AU - Tomberg, Eemeli
PY - 2024/9/20
Y1 - 2024/9/20
N2 - We study the formation of primordial black holes (PBHs) with ultraslow-roll inflation when stochastic effects are important. We use the ΔN formalism and simplify the stochastic equations with an analytical constant-roll approximation. Considering a viable inflation model, we find the spatial profile of the PBH compaction function numerically for each stochastic patch, without assumptions about Gaussianity or the radial profile. The stochastic effects that lead to an exponential tail for the density distribution also make the compaction function very spiky, unlike as assumed in the literature. Naively using collapse thresholds found for smooth profiles, the PBH abundance is enhanced by up to a factor of 109, and the PBH mass distribution is spread over 3 orders of magnitude in mass. The results point to a need to redo numerical simulations of PBH formation with spiky profiles. Published by the American Physical Society 2024
AB - We study the formation of primordial black holes (PBHs) with ultraslow-roll inflation when stochastic effects are important. We use the ΔN formalism and simplify the stochastic equations with an analytical constant-roll approximation. Considering a viable inflation model, we find the spatial profile of the PBH compaction function numerically for each stochastic patch, without assumptions about Gaussianity or the radial profile. The stochastic effects that lead to an exponential tail for the density distribution also make the compaction function very spiky, unlike as assumed in the literature. Naively using collapse thresholds found for smooth profiles, the PBH abundance is enhanced by up to a factor of 109, and the PBH mass distribution is spread over 3 orders of magnitude in mass. The results point to a need to redo numerical simulations of PBH formation with spiky profiles. Published by the American Physical Society 2024
U2 - 10.1103/physrevlett.133.121403
DO - 10.1103/physrevlett.133.121403
M3 - Journal article
VL - 133
JO - Physical review letters
JF - Physical review letters
SN - 0031-9007
IS - 12
M1 - 121403
ER -