TASI Lectures on Early Universe Cosmology: Inflation, Baryogenesis and Dark Matter

Cline, James M.

doi:10.22323/1.333.0001

Cited by 24 publications

(18 citation statements)

References 142 publications

(210 reference statements)

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“…The direct detection of gravitational waves [3] has triggered renewed interest in the role black holes might play in connection with these two outstanding open questions (see e.g. [4][5][6] and references therein). The idea that black hole evaporation can lead to the production of particles in the early universe and possibly to the generation of a baryon asymmetry or of dark matter has a rather long history.…”

mentioning

confidence: 99%

Melanopogenesis: dark matter of (almost) any mass and baryonic matter from the evaporation of primordial black holes weighing a ton (or less)

Morrison

Profumo

Yan

2019

J. Cosmol. Astropart. Phys.

138

122

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The evaporation of primordial black holes with a mass in the 1 gram M PBH 1000 kg range can lead to the production of dark matter particles of almost any mass in the range 0.1 MeV m DM 10 18 GeV with the right relic density at very early times, τ 10 −10 s. We calculate, as a function of the primordial black holes mass and initial abundance, the combination of dark matter particle masses and number of effective dark degrees of freedom leading to the right abundance of dark matter today, whether or not evaporation stops around the Planck scale. In addition, since black hole evaporation can also lead to the production of a baryon asymmetry, we calculate where dark matter production and baryogenesis can concurrently happen, under a variety of assumptions: baryogenesis via grand unification boson decay, via leptogenesis, or via asymmetric co-genesis of dark matter and ordinary matter. Finally, we comment on possible ways to test this scenario.

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mentioning

confidence: 99%

Melanopogenesis: dark matter of (almost) any mass and baryonic matter from the evaporation of primordial black holes weighing a ton (or less)

Morrison

Profumo

Yan

2019

J. Cosmol. Astropart. Phys.

138

122

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“…Using the definition of t f , we find that 16) which can be used to compute t f , once the form of Γ (t) is known. Thus we find that h(t) takes a very simple form, namely h(t) = exp − e β(t−t f ) .…”

Section: Wall Speedmentioning

confidence: 99%

“…(8.3). In practice, one evolves an unconstrained symmetric tensor u i j with the tensor source 16) and projects out the transverse traceless part h i j (t, k) from the Fourier transform u kl (t, k) with the appropriate projector. In the bubbles of a thermal transition, the scalar field part of the source is confined to a microscopically thin wall, while the fluid source is distributed over a significant volume.…”

Section: Gws From First-order Phase Transitionsmentioning

confidence: 99%

Phase transitions in the early universe

Hindmarsh

Lüben

Lumma

et al. 2021

SciPost Phys. Lect. Notes

165

169

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These lecture notes are based on a course given by Mark Hindmarsh at the 24th Saalburg Summer School 2018 and written up by Marvin Lüben, Johannes Lumma and Martin Pauly. The aim is to provide the necessary basics to understand first-order phase transitions in the early universe, to outline how they leave imprints in gravitational waves, and advertise how those gravitational waves could be detected in the future. A first-order phase transition at the electroweak scale is a prediction of many theories beyond the Standard Model, and is also motivated as an ingredient of some theories attempting to provide an explanation for the matter-antimatter asymmetry in our Universe. Starting from bosonic and fermionic statistics, we derive Boltzmann's equation and generalise to a fluid of particles with field dependent mass. We introduce the thermal effective potential for the field in its lowest order approximation, discuss the transition to the Higgs phase in the Standard Model and beyond, and compute the probability for the field to cross a potential barrier. After these preliminaries, we provide a hydrodynamical description of first-order phase transitions as it is appropriate for describing the early Universe. We thereby discuss the key quantities characterising a phase transition, and how they are imprinted in the gravitational wave power spectrum that might be detectable by the space-based gravitational wave detector LISA in the 2030s.

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“…The Standard Model (SM) as a gauge theory for elementary particle interactions has been extremely successful in explaining many phenomena. However, some issues including the matter-antimatter asymmetry of the Universe, the Dark Matter (DM) and hierarchy problem have remained unresolved [1][2][3][4]. These shortcomings imply that the SM is incomplete and needs to be extended.…”

Section: Introductionmentioning

confidence: 99%

Matter and dark matter asymmetry from a composite Higgs model

Ahmadvand

2021

Eur. Phys. J. C

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We propose a low scale leptogenesis scenario in the framework of composite Higgs models supplemented with singlet heavy neutrinos. One of the neutrinos can also be considered as a dark matter candidate whose stability is guaranteed by a discrete $${\mathbb {Z}}_2 $$ Z 2 symmetry of the model. In the spectrum of the strongly coupled system, bound states heavier than the pseudo Nambu–Goldstone Higgs boson can exist. Due to the decay of these states to heavy right-handed neutrinos, an asymmetry in the visible and dark sector is simultaneously generated. The resulting asymmetry is transferred to the standard model leptons which interact with visible right-handed neutrinos. We show that the sphaleron-induced baryon asymmetry can be provided at the TeV scale for resonant bound states. Depending on the coupling strength of dark neutrino interaction, a viable range of the dark matter mass is allowed in the model. Furthermore, taking into account the effective interactions of dark matter, we discuss low-energy processes and experiments.

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TASI Lectures on Early Universe Cosmology: Inflation, Baryogenesis and Dark Matter

Cited by 24 publications

References 142 publications

Melanopogenesis: dark matter of (almost) any mass and baryonic matter from the evaporation of primordial black holes weighing a ton (or less)

Melanopogenesis: dark matter of (almost) any mass and baryonic matter from the evaporation of primordial black holes weighing a ton (or less)

Phase transitions in the early universe

Matter and dark matter asymmetry from a composite Higgs model

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