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Dissecting the growth of the power spectrum for primordial black holes

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arxiv 1907.05237 v2 pith:JJDIGQW5 submitted 2019-07-11 astro-ph.CO gr-qchep-phhep-th

classification astro-ph.COgr-qchep-phhep-th
keywords growthpowerspectrumblackcannotconsiderexplanationholes
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

We consider the steepest rate at which the power spectrum from single field inflation can grow, with the aim of providing a simple explanation for the $k^4$ growth found recently. With this explanation in hand we show that a slightly steeper $k^5 (\log k )^2$ growth is in fact possible. Moreover, we argue that the power spectrum after a steep growth cannot immediately decay, but must remain large for the $k$ modes which exit during a $\sim2$ e-fold period. We also briefly consider how a strong growth can affect the spectral index of longer wavelengths preceding the growth, and show that even the conversion of isocurvature modes likely cannot lead to a stronger growth. These results have implications for the formation of primordial black holes, and other phenomena which require a large amplitude of power spectrum at short scales.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Axion USR Inflation

    astro-ph.CO 2025-07 conditional novelty 6.0 of 10

    In axion inflation with an intermediate ultra-slow-roll phase, the instability parameter collapses at the start of USR, terminating gauge production and yielding a two-peak power spectrum with P_R ∝ k^m, m>4.

  2. Inflationary magnetogenesis beyond slow-roll and its induced gravitational waves

    astro-ph.CO 2025-07 conditional novelty 6.0 of 10

    In the Ratra inflationary magnetogenesis model, a brief non-slow-roll phase amplifies the magnetic field power spectrum with maximal slope 4.75, and the induced gravitational wave background has a characteristic plate...

  3. Evolution of Linear Perturbations under Time-Dependent Hubble Friction I: SR-USR-SR Inflation

    gr-qc 2026-02 conditional novelty 5.0 of 10

    Analytic asymptotics show the dip in the SR-USR-SR curvature power spectrum comes from cancellation between two growing modes, not a constant-versus-growing cancellation.

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