Inflation and primordial black holes as dark matter

Ivanov, P. B.; Naselsky, P.; Новиков, И. Д.

doi:10.1103/physrevd.50.7173

Cited by 465 publications

(471 citation statements)

References 27 publications

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“…It is seen that the comoving mass decreases with time (M h < M ) (see, e.g., [51]). From (13,16) one has the expression for the function f for the Carr-Hawking collapse:…”

Section: A General Formulamentioning

confidence: 99%

“…In particular, in [15] the inflationary model with a steplike power spectrum based on a nonanalyticity in the inflaton potential was proposed and in subsequent works the inflationary potentials of such kind were used for making predictions of PBH production [16,17,18]. A step feature in the potential is an effective field theory description of a phase transition, so, in a more realistic approach an inflationary model should certainly involve more than one scalar field, and such rapid phenomena as phase transitions [19].…”

Section: Introductionmentioning

confidence: 99%

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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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“…It is seen that the comoving mass decreases with time (M h < M ) (see, e.g., [51]). From (13,16) one has the expression for the function f for the Carr-Hawking collapse:…”

Section: A General Formulamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Constraints on amplitudes of curvature perturbations from primordial black holes

Bugaev

Klimai

2009

Phys. Rev. D

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“…The situation will be drastically different in a BSI model, as will become clear from the results presented here. PBH production from models with a scale was considered before [13,14,15], but we shall reconsider it here in the light of our improved formulae from [7].…”

Section: Introductionmentioning

confidence: 99%

Accurate results for primordial black holes from spectra with a distinguished scale

et al. 2003

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We perform an accurate computation of the production rate for primordial black holes (PBHs). The reason is that the underlying mass variance had been overestimated systematically, as was shown recently. For scale-free powerlaw primordial spectra, and for a Universe with critical density, the mass variance is less than 34% of its value thought earlier for the spectral index in the range 1 ≤ n ≤ 1.3. We then extend our study to spectra with a characteristic scale and find the accurate shape of the corresponding mass variance. For a pure step in the primordial spectrum, the step in the variance is smoothed around the characteristic scale ks. For a spectrum with large oscillations near ks, we find a pronounced bump in the variance. This could yield a significant part of the cold dark matter in the form of PBHs with mass M in the range 5 × 10 15 g M 10 21 g.

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“…Significant bumps in the observable part of the spectrum are excluded though one may introduce them at very large k, close to the end of inflation, to obtain a significant number of primordial black holes (PBH), see e.g. [19,20]). If the size of the step is very small, the bump disappears and only a burst of oscillations remains.…”

Section: Introductionmentioning

confidence: 99%

New universal local feature in the inflationary perturbation spectrum

2008

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A model is developed in which the inflaton potential experiences a sudden small change in its second derivative (the effective mass of the inflaton). An exact treatment demonstrates that the resulting density perturbation has a quasi-flat power spectrum with a break in its slope (a step in ns). The step in the spectral index is modulated by characteristic oscillations and results in large running of the spectral index localised over a few e-folds of scales. A field-theoretic model giving rise to such behaviour of the inflationary potential is based on a fast phase transition experienced by a second scalar field weakly coupled to the inflaton. Such a transition is similar to that which terminates inflation in the hybrid inflationary scenario. This scenario suggests that the observed running of the spectral index in the WMAP data may be caused by a fast second order phase transition which occurred during inflation.

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Inflation and primordial black holes as dark matter

Cited by 465 publications

References 27 publications

Constraints on amplitudes of curvature perturbations from primordial black holes

Constraints on amplitudes of curvature perturbations from primordial black holes

Accurate results for primordial black holes from spectra with a distinguished scale

New universal local feature in the inflationary perturbation spectrum

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