Inflationary baryogenesis in a model with gauged baryon number

Barrie, Neil D.; Kobakhidze, Archil

doi:10.1007/jhep09(2014)163

Cited by 18 publications

(14 citation statements)

References 16 publications

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“…Universe and is initially present (as in asymmetric dark matter models) in both the visible and dark matter sector (see e.g. [7][8][9][10][11][12][13][14][15]). The asymmetry in this case would be carried either by Φ or by the primordial states -the difference from asymmetric dark matter simply being the later dilution.…”

Section: A Particle Asymmetry Comes Either From Inflaton Decays or Frmentioning

confidence: 99%

Flooded Dark Matter and S level rise

Randall

Scholtz

Unwin

2016

J. High Energ. Phys.

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Most dark matter models set the dark matter relic density by some interaction with Standard Model particles. Such models generally assume the existence of Standard Model particles early on, with the dark matter relic density a later consequence of those interactions. Perhaps a more compelling assumption is that dark matter is not part of the Standard Model sector and a population of dark matter too is generated at the end of inflation. This democratic assumption about initial conditions does not necessarily provide a natural value for the dark matter relic density, and furthermore superficially leads to too much entropy in the dark sector relative to ordinary matter. We address the latter issue by the late decay of heavy particles produced at early times, thereby associating the dark matter relic density with the lifetime of a long-lived state. This paper investigates what it would take for this scenario to be compatible with observations in what we call Flooded Dark Matter (FDM) models and discusses several interesting consequences. One is that dark matter can be very light and furthermore, light dark matter is in some sense the most natural scenario in FDM as it is compatible with larger couplings of the decaying particle. A related consequence is that the decay of the field with the smallest coupling and hence the longest lifetime dominates the entropy and possibly the matter content of the Universe, a principle we refer to as "Maximum Baroqueness". We also demonstrate that the dark sector should be colder than the ordinary sector, relaxing the most stringent free-streaming constraints on light dark matter candidates. We will discuss the potential implications for the core-cusp problem in a follow-up paper. The FDM framework will furthermore have interesting baryogenesis implications. One possibility is that dark matter is like the baryon asymmetry and both are simultaneously diluted by a late entropy dump. Alternatively, FDM is compatible with an elegant non-thermal leptogenesis implementation in which decays of a heavy right-handed neutrino lead to late time reheating of the Standard Model degrees of freedom and provide suitable conditions for creation of a lepton asymmetry.

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Section: A Particle Asymmetry Comes Either From Inflaton Decays or Frmentioning

confidence: 99%

Flooded Dark Matter and S level rise

Randall

Scholtz

Unwin

2016

J. High Energ. Phys.

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“…In Ref. [40], the authors considered the extension of the Standard Model with anomalous gauge symmetry. They obtained the required BAU for H Inf ∼ 10 14 GeV and reheating temperate at 10 16 GeV.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…In the early Universe, the generation of the non-zero helical magnetic fields leads to a chiral anomaly resulting from the imbalance between left and right-handed fermions. In the presence of an electromagnetic field in curved space-time, the chiral anomaly is given by the following equation [39,40]:…”

Section: Conditions On Baryogenesis In the Presence Of Magnetic Fieldmentioning

confidence: 99%

Helical magnetic fields from Riemann coupling

Kushwaha

Shankaranarayanan

2020

Phys. Rev. D

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The spectrum of energy density fluctuations, baryon asymmetry, and coherent large-scale magnetic fields are the three observables that provide crucial information on physics at very high energies. Inflation can only provide a mechanism to explain the density perturbations, and the origin of primordial magnetic fields and baryon asymmetry require physics beyond the standard models of cosmology and particle physics. In this work, we show that the mechanism that leads to primordial helical fields also leads to baryogenesis at the beginning of the radiation-dominated epoch. The model we consider here consists of mass dimension 6 operators that include Riemann coupling between gravity and electromagnetic field without extending the Standard Model of particle physics. We explicitly show that the generation of helical magnetic fields leads to baryogenesis.We further show that the model predicts the observed amount of baryon asymmetry of the Universe for a range of reheating temperatures consistent with the observations.

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“…Even if the pseudoscalar coupling only leads to weak breaking of Weyl invariance, it efficiently modifies the topological properties of the hypermagnetic flux lines in the electroweak plasma [25], as as originally discussed in [26] by taking into account the chemical potentials associated with the finite density effects. If the gyrotropy sufficiently large the produced Chern-Simons condensates may decay and eventually produce the baryon asymmetry [26,27,[29][30][31][32]. These gyrotropic and helical fields play also a key role in various aspects of anomalous magnetohydrodynamics [33].…”

Section: Introductionmentioning

confidence: 99%

“…For this reason the production of the BAU demands, in this context, the dynamical generation of the gyrotropic configurations of the hypermagnetic field as argued, in Refs. [25,26] (see also [27,[29][30][31]). Even if the idea explored here is admittedly less conventional it certainly provides a useful playground for the potential unification of the baryogenesis conditions and of the magnetogenesis requirements.…”

Section: Introductionmentioning

confidence: 99%

Baryogenesis, magnetogenesis and the strength of anomalous interactions

Giovannini

2021

Eur. Phys. J. C

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The production of the hypermagnetic gyrotropy is investigated under the assumption that the gauge coupling smoothly evolves during a quasi-de Sitter phase and then flattens out in the radiation epoch by always remaining perturbative. In the plane defined by the strength of the anomalous interactions and by the rate of evolution of the gauge coupling the actual weight of the pseudoscalar interactions turns out to be always rather modest if major deviations from the homogeneity are to be avoided during the inflationary phase. Even if the gauge power spectra are related by duality only in the absence of anomalous contributions, an approximate duality symmetry constrains the late-time form of the hypermagnetic power spectra. Since the hypermagnetic gyrotropy associated with the modes reentering prior to the phase transition must be released into fermions later on, the portions of the parameter space where the obtained baryon asymmetry is close to the observed value are the most relevant for the present ends. For the same range of parameters the magnetic power spectra associated with the modes reentering after symmetry breaking may even be of the order of a few hundredths of a nG over typical length scales comparable with the Mpc prior to the collapse of the protogalaxy.

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Inflationary baryogenesis in a model with gauged baryon number

Cited by 18 publications

References 16 publications

Flooded Dark Matter and S level rise

Flooded Dark Matter and S level rise

Helical magnetic fields from Riemann coupling

Baryogenesis, magnetogenesis and the strength of anomalous interactions

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