Dynamics of the electroweak phase transition

Carrington, M. E.; Kapusta, Joseph I.

doi:10.1103/physrevd.47.5304

Cited by 50 publications

(71 citation statements)

References 41 publications

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“…In order are the issue of the type of the phase transition, depending on the Higgs mass, or the right form of potential temperature correction terms, see Refs. [33,34]. In the present theory, however, the vacuum energy is very large, V 1/4 ∼ √ M P l M H χ, because of the gravity non-minimal coupling, which acts like a negative mass term to induce the phase transition; for a similar view in the context of the SU(5) GUT see Ref.…”

Section: Frw-modelsmentioning

confidence: 94%

Induced gravity inflation in the standard model of particle physics

1995

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We are considering the cosmological consequences of an induced gravity theory coupled to the minimal standard model of particle physics. The non-minimal coupling parameter between gravity and the Higgs field must then be very large, yielding some new cosmological consequences for the early Universe and new constraints on the Higgs mass. As an outcome, new inflation is only possible for very special initial conditions producing first a short contraction era after which an inflationary expansion automatically follows; a chaotic inflationary scenario is successfully achieved. The contrast of density perturbations required to explain the seed of astronomic structures are obtained for very large values of the Higgs mass (M H >> G −1/2 F ), otherwise the perturbations have a small amplitude; in any case, the spectral index of scalar perturbations agrees with the observed one.

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Section: Frw-modelsmentioning

confidence: 94%

Induced gravity inflation in the standard model of particle physics

1995

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“…Building on previous work [26,[71][72][73][74][75], Moore and Prokopec were the first to calculate the velocity for the Standard Model case microphysically in refs. [76,77] (ref.…”

Section: Jhep10(2015)135mentioning

confidence: 99%

Bubble expansion and the viability of singlet-driven electroweak baryogenesis

Kozaczuk

2015

J. High Energ. Phys.

139

146

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The standard picture of electroweak baryogenesis requires slowly expanding bubbles. This can be difficult to achieve if the vacuum expectation value (VEV) of a gauge singlet scalar field changes appreciably during the electroweak phase transition. It is important to determine the bubble wall velocity in this case, since the predicted baryon asymmetry can depend sensitively on its value. Here, this calculation is discussed and illustrated in the real singlet extension of the Standard Model. The friction on the bubble wall is computed using a kinetic theory approach and including hydrodynamic effects. Wall velocities are found to be rather large (v w 0.2) but compatible with electroweak baryogenesis in some portions of the parameter space. If the phase transition is strong enough, however, a subsonic solution may not exist, precluding non-local electroweak baryogenesis altogether. The results presented here can be used in calculating the baryon asymmetry in various singlet-driven scenarios, as well as other features related to cosmological phase transitions in the early Universe, such as the resulting spectrum of gravitational radiation.

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“…The third and most relevant estimate is the mean time between two-body collisions in the standard model for temperatures greater than the electroweak symmetry restoration temperature. This mean time was calculated in [14] in the process of calculating the viscosity in the relaxation time approximation. Averaged over all particle species in the standard model one may infer from that paper an average time of 3.7/T .…”

Section: Numerical Solution and Scalingmentioning

confidence: 99%

“…Now we turn to the viscosities. The shear viscosity was calculated in [14] for the full standard model in the symmetry restored phase, meaning temperatures above 100 GeV or so, using the relaxation time approximation. The result is η(T > 100 GeV) = 82.5 T 3 (12) when numerical values for coupling constants etc.…”

Section: Equation Of State and Transport Coefficientsmentioning

confidence: 99%

High temperature matter and gamma ray spectra from microscopic black holes

Daghigh

Kapusta

2002

Phys. Rev. D

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The relativistic viscous fluid equations describing the outflow of high temperature matter created via Hawking radiation from microscopic black holes are solved numerically for a realistic equation of state. We focus on black holes with initial temperatures greater than 100 GeV and lifetimes less than 6 days. The spectra of direct photons and photons from π 0 decay are calculated for energies greater than 1 GeV. We calculate the diffuse gamma ray spectrum from black holes distributed in our galactic halo. However, the most promising route for their observation is to search for point sources emitting gamma rays of ever-increasing energy.

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Dynamics of the electroweak phase transition

Cited by 50 publications

References 41 publications

Induced gravity inflation in the standard model of particle physics

Induced gravity inflation in the standard model of particle physics

Bubble expansion and the viability of singlet-driven electroweak baryogenesis

High temperature matter and gamma ray spectra from microscopic black holes

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