SUSY variants of the electroweak phase transition

Huber, Stephan J.; Schmidt, Michael G.

doi:10.1007/s100529900135

Cited by 34 publications

(44 citation statements)

References 42 publications

(64 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A second way to make the EWPT more strongly first-order is to couple the Higgs to a new scalar that develops a VEV near the electroweak scale [88][89][90][91][92][93][94]. A simple example of this is…”

Section: Extending the Standard Model Scalar Sectormentioning

confidence: 99%

Electroweak baryogenesis

2012

View full text Add to dashboard Cite

Abstract. Electroweak baryogenesis (EWBG) remains a theoretically attractive and experimentally testable scenario for explaining the cosmic baryon asymmetry. We review recent progress in computations of the baryon asymmetry within this framework and discuss their phenomenological consequences. We pay particular attention to methods for analyzing the electroweak phase transition and calculating CP-violating asymmetries, the development of Standard Model extensions that may provide the necessary ingredients for EWBG, and searches for corresponding signatures at the high energy, intensity and cosmological frontiers.

show abstract

Section: Extending the Standard Model Scalar Sectormentioning

confidence: 99%

Electroweak baryogenesis

2012

View full text Add to dashboard Cite

show abstract

“…Besides, while the Standard Model predicts a smooth cross-over for this transition, its extensions can give a strong first-order phase transition, which is a fundamental ingredient for electroweak baryogenesis and the generation of primordial magnetic fields. 19 Supersymmetric extensions of the Standard Model have been the most intensively studied [208,209,210,211,212,213], but it is also possible to get a strong transition from more generic two-Higgs doublet models [214,215], from technicolor theories [216], etc. [8][9][10][11][12][13][14][15][16][17] [217,218,219,220].…”

Section: Magnetogenesis In Phase Transitionsmentioning

confidence: 99%

Primordial magnetogenesis

Kandus¹,

Kunze²,

Tsagas³

2011

Physics Reports

337

423

View full text Add to dashboard Cite

Magnetic fields appear everywhere in the universe. From stars and galaxies, all the way to galaxy clusters and remote protogalactic clouds magnetic fields of considerable strength and size have been repeatedly observed. Despite their widespread presence, however, the origin of cosmic magnetic fields is still a mystery. The galactic dynamo is believed capable of amplifying weak magnetic seeds to strengths like those measured in ours and other galaxies, but the question is where do these seed fields come from? Are they a product of late, post-recombination, physics or are they truly cosmological in origin? The idea of primordial magnetism is attractive because it makes the large-scale magnetic fields, especially those found in early protogalactic systems, easier to explain. As a result, a host of different scenarios have appeared in the literature. Nevertheless, early magnetogenesis is not problem free, with a number of issues remaining open and a matter of debate. We review the question of primordial magnetic fields and consider the limits set on their strength by the current observational data. The various mechanisms of pre-recombination magnetogenesis are presented and their advantages and shortcomings are debated. We consider both classical and quantum scenarios, that operate within as well as outside the standard model, and also discuss how future observations could be used to decide whether the large-scale magnetic fields we see in the universe today are truly primordial or not.Comment: 107 pages, 3 figures. Revised and expanded version, to be published in Physics Report

show abstract

“…This feature is independent of the concrete embeddings of the sMSSM, though we are using an effective potential of finite temperature in Model I as an illustration. This feature is also shared by the NMSSM [43,44,45,46], the nMSSM [51,52], the U(1) ′ models with no secluded sector [89], and the singlet extensions of the SM [21].…”

Section: The Electroweak Phase Transitionmentioning

confidence: 99%

“…In the Next-to-Minimal Supersymmetric Standard Model (NMSSM) [42] there is a trilinear term A h hSH u H d in the Higgs potential, where S is a singlet under the SM gauge group. This allows a strong enough first order EWPT [43,44,45,46]. In the best-motivated versions of the NMSSM (motivated by the µ problem [47]), the effective µ parameter is given by h S (for recent studies, see [48]).…”

Section: Introductionmentioning

confidence: 99%

“…However, the original versions involve a discrete Z 3 symmetry and serious cosmological domain wall problems [49]. These can be avoided by introducing an elementary bilinear µ term in the superpotential (or linear or quadratic terms in S), but at the cost of reintroducing the µ (or analogous) problems [44,45]. The domain wall problem can also be avoided in an alternative version of the NMSSM [50], and in the nearly Minimal Supersymmetric Standard Model (nMSSM) [51,52,53], using a different discrete symmetry broken by a loopinduced tadpole.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Electroweak baryogenesis, CDM and anomaly-free supersymmetric U(1)′ models

Kang¹,

Langacker²,

et al. 2011

J. High Energ. Phys.

View full text Add to dashboard Cite

We construct two anomaly-free supersymmetric U (1) ′ models with a secluded U (1) ′ -breaking sector. For the one with E 6 embedding we show that there exists a strong enough first order electroweak phase transition for electroweak baryogenesis (EWBG) because of the large soft trilinear terms in the Higgs potential. Unlike the Minimal Supersymmetric Standard Model (MSSM), the stop masses can be very heavy. We then discuss possible CP violation in the Higgs sector, which can be both spontaneous and explicit, even at tree level. The spontaneous violation provides a direct source for baryogenesis, while its magnitude is mediated by an explicit phase from the secluded sector. These new CP sources do not introduce significant new contributions to electric dipole moments. EWBG in the thin wall (τ leptons) and thick wall regimes (top squarks, charginos and top quarks) are systematically discussed. We find that the CP -violating stop and chargino currents are very different from those obtained in the MSSM. Due to the space-dependence of the relevant CP phases, they do not require a variation of tan β in the bubble wall to have a non-trivial structure at the lowest order of Higgs insertion. In addition to τ leptons, top squarks and charginos, we find that top quarks can also play a significant role. Numerical results show that the baryon asymmetry is large enough to explain the cosmological observation today. We illustrate that EWBG and neutralino cold dark matter can be accommodated in the same framework, i.e., there exists parameter space where a strong enough first order EWPT, large CP phase variations across the bubble wall, a reasonable baryon asymmetry as well as an acceptable neutralino dark matter relic density can be achieved simultaneously.

show abstract

SUSY variants of the electroweak phase transition

Cited by 34 publications

References 42 publications

Electroweak baryogenesis

Electroweak baryogenesis

Primordial magnetogenesis

Electroweak baryogenesis, CDM and anomaly-free supersymmetric U(1)′ models

Contact Info

Product

Resources

About