Quantum transport and electroweak baryogenesis

Konstandin, Thomas

doi:10.3367/ufne.0183.201308a.0785

Cited by 111 publications

(62 citation statements)

References 153 publications

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“…Including gradient effects appears to recover some of the resonance [425]. When various approaches to calculating CP violating sources is valid remains an open problem in the field [426]. Since the standard model fails on two accounts to satisfy the Sakharov conditions, it is typical to extend the standard model by two sectors -one sector which catalyzes the electroweak phase transition, and another which is responsible for CP violating interactions with the bubble wall.…”

Section: And Cp Violation (One or The Other Is Insufficient)mentioning

confidence: 99%

Review of cosmic phase transitions: their significance and experimental signatures

Mazumdar

White²

2019

Rep. Prog. Phys.

206

195

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The study of cosmic phase transitions are of central interest in modern cosmology. In the standard model of cosmology the Universe begins in a very hot state, right after at the end of inflation via the process of reheating/preheating, and cools to its present temperature as the Universe expands. Both new and existing physics at any scale can be responsible for catalyzing either first, second or cross over phase transition, which could be either thermal or non-thermal with a potential observable imprints. Thus this field prompts a rich dialogue between gravity, particle physics and cosmology. It is all but certain that at least two cosmic phase transitions have occurred -the electroweak and the QCD phase transitions. The focus of this review will be primarily on phase transitions above such scales, We review different types of phase transitions that can appear in our cosmic history, and their applications and experimental signatures in particular in the context of exciting gravitational waves, which could be potentially be constrained by LIGO/VIRGO, Kagra, and eLISA.Let us briefly summarize the early Universe cosmology in chronological order. How the Universe began remains a profound question, for which we do not have direct experimental evidence yet. Nonetheless, we can speculate based on sound physical arguments and the observations confirmed by the detection of cosmic microwave background (CMB) radiation [46,47]. How did the Universe begin?Einstein's theory of gravity (GR) is extremely successful in the infrared (IR) matching of all possible observables [48], including the recent discovery of gravitational waves from mergers of two blackholes [49], and binary neutron star mergers [50]. However at short distances and small time scales, i.e. in the ultraviolet (UV), GR has pathologies, besides being a non-renormalizable theory, GR introduces cosmological and blackhole singularities, see [51], and in some cases naked singularities, see [52]. In GR, our Universe has a distinct starting point, a singular spacetime -as long as all the standard energy conditions are always satisfied, i.e. strong, weak, and null energy conditions, see [51]. It is possible to address the cosmological singularity problem without violating the matter energy conditions by weakening the gravitational interaction in the UV. This can happen in ghost free infinite derivative gravity inspired from string field theory [53,54]. There could be two consequences for such study; one could be a realization of a non-singular bounce [55,56], and the other scenario would be that Universe could be frozen in time in the UV, such that the Universe becomes conformal as t → 0 [57]. Bouncing cosmologies and cosmological density perturbations have been reviewed in this nice review [58,59]. There is a strong indication that this non-singular initial phase of the Universe has a key role to play towards understanding the subsequent phases of the Universe such as cosmic inflation, horizon, homogeneity and isotropy of the Universe , to create appropriate initial co...

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Section: And Cp Violation (One or The Other Is Insufficient)mentioning

confidence: 99%

Review of cosmic phase transitions: their significance and experimental signatures

Mazumdar

White²

2019

Rep. Prog. Phys.

206

195

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“…Interestingly, this model exhibits a range of parameters for which the PT is long-lasting, meaning that most of the true vacuum bubbles are nucleated around T ∼ 50 GeV but collide well below the electroweak scale, as low as T ∼ [0. 1,10] GeV. Precise results depend on the exact equation of the state of the Universe which is complicated to compute in this context.…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from a supercooled electroweak phase transition and their detection with pulsar timing arrays

et al. 2017

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We investigate the properties of a stochastic gravitational wave background produced by a first-order electroweak phase transition in the regime of extreme supercooling. We study a scenario whereby the percolation temperature that signifies the completion of the transition, T p , is as low as a few MeV (nucleosynthesis temperature), while most of the true vacuum bubbles are formed much earlier at the nucleation temperature, T n ∼ 50 GeV. This implies that the gravitational wave spectrum is mainly produced by the collisions of large bubbles and characterised by a large amplitude and a peak frequency as low as f ∼ 10 −9 −10 −7 Hz. We show that such a scenario can occur in (but not limited to) a model based on a non-linear realisation of the electroweak gauge group, so that the Higgs vacuum configuration is altered by a cubic coupling. In order to carefully quantify the evolution of the phase transition of this model over such a wide temperature range we go beyond the usual fast transition approximation, taking into account the expansion of the Universe as well as the behaviour of the nucleation probability at low temperatures. Our computation shows that there exists a range of parameters for which the gravitational wave spectrum lies at the edge between the exclusion limits of current pulsar timing array experiments and the detection band of the future Square Kilometre Array observatory.

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“…Among the most theoretically attractive and phenomenologically testable is electroweak baryogenesis (EWBG) [3] (for reviews, see Refs. [4][5][6][7][8][9][10][11][12]). EWBG proceeds via bubble nucleation during a first-order electroweak phase transition (EWPT), providing the needed outof-equilibrium conditions.…”

Section: Introductionmentioning

confidence: 99%

Standard model with a complex scalar singlet: Cosmological implications and theoretical considerations

2018

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We analyze the theoretical and phenomenological considerations for the electroweak phase transition and dark matter in an extension of the standard model with a complex scalar singlet (cxSM). In contrast with earlier studies, we use a renormalization group improved scalar potential and treat its thermal history in a gauge-invariant manner. We find that the parameter space consistent with a strong first-order electroweak phase transition (SFOEWPT) and present dark matter phenomenological constraints is significantly restricted compared to results of a conventional, gauge-noninvariant analysis. In the simplest variant of the cxSM, recent LUX data and a SFOEWPT require a dark matter mass close to half the mass of the standard model-like Higgs boson. We also comment on various caveats regarding the perturbative treatment of the phase transition dynamics.

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Quantum transport and electroweak baryogenesis

Cited by 111 publications

References 153 publications

Review of cosmic phase transitions: their significance and experimental signatures

Review of cosmic phase transitions: their significance and experimental signatures

Gravitational waves from a supercooled electroweak phase transition and their detection with pulsar timing arrays

Standard model with a complex scalar singlet: Cosmological implications and theoretical considerations

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