Forming sub-horizon black holes at the end of inflation

Lyth, David H.; Malik, Karim A.; Sasaki, Misao; Zaballa, Ignacio

doi:10.1088/1475-7516/2006/01/011

Cited by 37 publications

(68 citation statements)

References 24 publications

(57 reference statements)

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“…[55]. We assume that reheating is rapid and, correspondingly, the moment of the end of inflation coincides with the moment of a beginning of the radiation epoch.…”

Section: Time Dependence Of the Gravitational Potentialmentioning

confidence: 99%

Constraints on amplitudes of curvature perturbations from primordial black holes

Bugaev

Klimai

2009

Phys. Rev. D

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We calculate the primordial black hole (PBH) mass spectrum produced from a collapse of the primordial density fluctuations in the early Universe using, as an input, several theoretical models giving the curvature perturbation power spectra PR(k) with large (∼ 10 −2 ÷ 10 −1 ) values at some scale of comoving wave numbers k. In the calculation we take into account the explicit dependence of gravitational (Bardeen) potential on time. Using the PBH mass spectra, we further calculate the neutrino and photon energy spectra in extragalactic space from evaporation of light PBHs, and the energy density fraction contained in PBHs today (for heavier PBHs). We obtain the constraints on the model parameters using available experimental data (including data on neutrino and photon cosmic backgrounds). We briefly discuss the possibility that the observed 511 keV line from the Galactic center is produced by annihilation of positrons evaporated by PBHs.

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“…[55]. We assume that reheating is rapid and, correspondingly, the moment of the end of inflation coincides with the moment of a beginning of the radiation epoch.…”

Section: Time Dependence Of the Gravitational Potentialmentioning

confidence: 99%

Constraints on amplitudes of curvature perturbations from primordial black holes

Bugaev

Klimai

2009

Phys. Rev. D

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“…We used this fact in Ref. [10] to give an estimate of the mass fraction of PBHs. Here in order to extend the calculation to scales of the order of the horizon scale at the end of inflation, we calculate B(x e ) numerically.…”

Section: B Pbh Abundancementioning

confidence: 99%

“…The Fourier components of the density contrast and the curvature perturbation are related by [25] 10) so that, at horizon crossing, P δ = (4/9)…”

Section: Figmentioning

confidence: 99%

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Constraints on the primordial curvature perturbation from primordial black holes

Zaballa

Green

Malik

et al. 2007

J. Cosmol. Astropart. Phys.

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We calculate the constraints on the primordial curvature perturbation at the end of inflation from the present day abundance of Primordial Black Holes (PBHs), as a function of the reheat temperature TRH. We first extend recent work on the formation of PBHs on scales which remain within the horizon during inflation and calculate the resulting constraints on the curvature perturbation. We then evaluate the constraint from PBHs that form, more conventionally, from super-horizon perturbations. The constraints apply for TRH < 10 8 GeV and the inclusion of sub-horizon PBHs leads to a limit which is roughly three times tighter than the bound from super-horizon PBHs.

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“…Here, R k ð i Þ is the Fourier component of the curvature perturbation on the comoving hypersurfaces at the end of inflation (see, e.g., [43]). The connection between values of the smoothing mass M, density contrast H R , and PBH mass M BH can be expressed in the general form…”

Section: Pbh Mass Spectrum Calculationmentioning

confidence: 99%

Constraints on the induced gravitational wave background from primordial black holes

2011

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We perform a consistent calculation of primordial black hole (PBH) mass spectrum and second-order induced gravitational wave (GW) background produced from primordial scalar perturbations in radiation era of the early Universe. It is shown that the maximal amplitudes of the second-order GW spectrum that can be approached without conflicting with the PBH data do not depend significantly on the shape of primordial perturbation spectrum. The constraints on the GW background obtained in previous works are extended to a wider GW frequency range. We discuss the applicability of the currently available pulsar timing limits for obtaining the constraints on scalar power spectrum and PBH abundance and show that they can be used for strongly constraining the PBH number density in the PBH mass range $ð0:03 À 10ÞM .

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Forming sub-horizon black holes at the end of inflation

Cited by 37 publications

References 24 publications

Constraints on amplitudes of curvature perturbations from primordial black holes

Constraints on amplitudes of curvature perturbations from primordial black holes

Constraints on the primordial curvature perturbation from primordial black holes

Constraints on the induced gravitational wave background from primordial black holes

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