Unification models with reheating via primordial black holes

Hidalgo, Juan Carlos; Ureña–López, L. Arturo; Liddle, Andrew R.

doi:10.1103/physrevd.85.044055

Cited by 42 publications

(31 citation statements)

References 54 publications

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“…The survival of nongravitational relics (including, for example and in addition to DM, matterantimatter asymmetry [57,58,59,60,61], primordial magnetic fields [62,63,64,65,66], or effective number of relativistic species [67,68]) will depend on the details of the expansion history and post-inflationary thermalization of radiation. Along with large-scale gravitational effects associated with the expansion history, smaller scale gravitational effects -including horizon-scaled variations of expansion history and associated non-Gaussianities [69,70,71,72,73,74,75,76,77,78], imprints from small-scale clustering of matter [43,79,80], PBHs [81,82,83,84,85,86,87,88,89,90,91,92,93], and gravitational waves resulting from violent nonlinear dynamics [94, 95, 96, 97, 98, 99, 100, 101, 102, 103, 104, 105] -provide hope for future observational probes of the time before BBN. All of the above aspects are topics of this paper.…”

Section: Introductionmentioning

confidence: 99%

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

Allahverdi¹,

Amin²,

Berlin³

et al. 2021

TheOJA

200

140

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It is commonly assumed that the energy density of the Universe was dominated by radiation between reheating after inflation and the onset of matter domination 54,000 years later. While the abundance of light elements indicates that the Universe was radiation dominated during Big Bang Nucleosynthesis (BBN), there is scant evidence that the Universe was radiation dominated prior to BBN. It is therefore possible that the cosmological history was more complicated, with deviations from the standard radiation domination during the earliest epochs. Indeed, several interesting proposals regarding various topics such as the generation of dark matter, matter-antimatter asymmetry, gravitational waves, primordial black holes, or microhalos during a nonstandard expansion phase have been recently made. In this paper, we review various possible causes and consequences of deviations from radiation domination in the early Universe -taking place either before or after BBN -and the constraints on them, as they have been discussed in the literature during the recent years.

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Section: Introductionmentioning

confidence: 99%

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

Allahverdi¹,

Amin²,

Berlin³

et al. 2021

TheOJA

200

140

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“…98,[238][239][240][241][242] If such black holes decay quickly, they would contribute to reheating the universe. If they survive for a long time, they would eventually dominate the radiation component, leading to a matter-dominated expansion history.…”

Section: Primordial Black Holesmentioning

confidence: 99%

Nonperturbative dynamics of reheating after inflation: A review

Amin

Hertzberg

Kaiser

et al. 2014

Int. J. Mod. Phys. D

450

492

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Our understanding of the state of the universe between the end of inflation and big bang nucleosynthesis (BBN) is incomplete. The dynamics at the end of inflation are rich and a potential source of observational signatures. Reheating, the energy transfer between the inflaton and Standard Model fields (possibly through intermediaries) and their subsequent thermalization, can provide clues to how inflation fits in with known high-energy physics. We provide an overview of our current understanding of the nonperturbative, nonlinear dynamics at the end of inflation, some salient features of realistic particle physics models of reheating, and how the universe reaches a thermal state before BBN. In addition, we review the analytical and numerical tools available in the literature to study preheating and reheating and discuss potential observational signatures from this fascinating era.

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“…Other interesting works consider a single scalar field to unify the description of dark matter, dark energy and inflation [70,71,54].…”

Section: Introductionmentioning

confidence: 99%