Cosmological consequences of slow-moving bubbles in first-order phase transitions

Davis, Anne-Christine; Lilley, Matthew

doi:10.1103/physrevd.61.043502

Cited by 20 publications

(31 citation statements)

References 22 publications

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“…Consequently, the size of the bubbles only increases at a speed parametrically determined by the rate Hubble expansion decreases the temperature of the universe. The thermodynamics of the situation have been studied in detail in [45,46], and it has also been proposed that a long lasting phase transition could significantly reduce the relic abundance of thermal dark matter candidates [47].…”

Section: Jhep02(2017)046mentioning

confidence: 99%

Miniclusters in the axiverse

Hardy

2017

J. High Energ. Phys.

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If dark matter is an axion-like-particle a significant fraction of the present day relic abundance could be concentrated in compact gravitationally bound miniclusters. We study the minicluster masses compatible with the dark matter relic density constraint. If they form from fluctuations produced by PQ symmetry breaking, minicluster masses up to hundreds of solar masses are possible, although over most of the parameter space they are much lighter. The size of these objects is typically within a few orders of magnitude of an astronomical unit. We also show that miniclusters can form if an axion gets mass from a hidden sector with a first order phase transition that takes a relatively long time to complete. Therefore they can appear in models where PQ symmetry is broken before inflation, compatible with large axion decay constants and string theory UV completions.

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Section: Jhep02(2017)046mentioning

confidence: 99%

Miniclusters in the axiverse

Hardy

2017

J. High Energ. Phys.

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“…The evolution and the collision of slow-moving true vacuum bubbles are examined in Ref. [22]. The comoving bubble walls prevent the formation of extra defects and may lead to an increase of any primordial magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Quark-hadron phase transitions in the viscous early universe

Tawfik

Harkó

2012

Phys. Rev. D

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In the standard hot big bang theory, when the Universe was about 1 − 10 µs old, the cosmological matter is conjectured to undergo Quantum Chromodynamics (QCD) phase transition(s) from quark matter to hadrons. In the present work, we study the cosmological quark-hadron phase transition in two different physical scenarios. First, by assuming that the phase transition would be described by an effective nucleation theory (prompt first-order phase transition), we analyze the evolution of the relevant cosmological parameters of the early Universe (energy density ρ, temperature T , Hubble parameter H and the scale factor a) before, during and after the phase transition. To study the cosmological dynamics and the time evolution, we use both analytical and numerical methods. The case where the Universe evolved through a mixed phase with a small initial supercooling and monotonically growing hadronic bubbles is also considered in detail. The numerical estimation of the cosmological parameters, a and H for instance, shows that the time evolution of the Universe varies from phase to phase. As the QCD era turns to be fairly accessible in the high-energy experiments and the lattice QCD simulations, the QCD equation of state is very well defined. In light of these QCD results, we develop a systematic study of the crossover quark-hadron phase transition and an estimation for the time evolution of the Hubble parameter during the crossover .

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“…As expected, the resulting field strength is of the order of M 2 W /g with a correlation length ξ ∼ M −1 W . However, when plasma friction and conductivity are taken into account, the magnetic field spreads over the interior of a bubble [30] leading to an appreciable increase in correlation length.…”

Section: Magnetic Fields From Bubble Collisionsmentioning

confidence: 99%

The Origin of Cosmic Magnetic Fields

Törnkvist

2000

Cosmo-99

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In this talk, I review a number of particle-physics models that lead to the creation of magnetic fields in the early universe and address the complex problem of evolving such primordial magnetic fields into the fields observed today. Implications for future observations of the Cosmic Microwave Background (CMB) are discussed. Focussing on first-order phase transitions in the early universe, I describe how magnetic fields arise in the collision of expanding true-vacuum bubbles both in Abelian and non-Abelian gauge theories.

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Cosmological consequences of slow-moving bubbles in first-order phase transitions

Cited by 20 publications

References 22 publications

Miniclusters in the axiverse

Miniclusters in the axiverse

Quark-hadron phase transitions in the viscous early universe

The Origin of Cosmic Magnetic Fields

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