RRR fluctuations from non-singular bounce
Abstract
We present a consistent treatment of regularization, renormalization, and resummation in a framework involving a contracting phase, a non-singular bounce, and inflation with a sharp transition from slow-roll to ultra-slow-roll, enabling primordial black hole production. Within an effective field theory approach, we compute quantum loop corrections to the power spectrum across all phases. Quadratic UV divergences are removed through renormalization, while logarithmic IR divergences are softened via resummation, demonstrating scheme independence. The inclusion of contraction and bounce allows the generation of solar-mass PBHs, MPBH∼cal O(M⊙), with minimal inflation ΔNTotal∼cal O(60), thereby evading the no-go theorem. For 0.88≤ cs≤1, the peak spectrum amplitude lies within 10−3≤ A≤10−2, preserving causality and unitarity. PBH abundances across 10−33 − 10−27 and 10−6 − 10−1M⊙ are confronted with microlensing constraints to control PBH overproduction.
Versions
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BibTeX
@misc{choudhury2026fluctuations,
title = {{RRR fluctuations from non-singular bounce}},
author = {Sayantan Choudhury},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.38990},
eprint = {2609.38990},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.38990},
}
RIS
TY - UNPB
TI - RRR fluctuations from non-singular bounce
AU - Sayantan Choudhury
PY - 2026
DA - 2026/09/30
PB - arXiv
DO - 10.48550/arxiv.2609.38990
UR - https://arxiv.org/abs/2609.38990
AB - We present a consistent treatment of regularization, renormalization, and resummation in a framework involving a contracting phase, a non-singular bounce, and inflation with a sharp transition from slow-roll to ultra-slow-roll, enabling primordial black hole production. Within an effective field theory approach, we compute quantum loop corrections to the power spectrum across all phases. Quadratic UV divergences are removed through renormalization, while logarithmic IR divergences are softened via resummation, demonstrating scheme independence. The inclusion of contraction and bounce allows the generation of solar-mass PBHs, M_PBH∼cal O(M_⊙), with minimal inflation ΔN_Total∼cal O(60), thereby evading the no-go theorem. For 0.88≤ c_s≤1, the peak spectrum amplitude lies within 10^−3≤ A≤10^−2, preserving causality and unitarity. PBH abundances across 10^−33 − 10^−27 and 10^−6 − 10^−1M_⊙ are confronted with microlensing constraints to control PBH overproduction.
ER -