Hypermagnetic fields and baryon asymmetry from pseudoscalar inflation

Anber, Mohamed M.; Sabancilar, Eray

doi:10.1103/physrevd.92.101501

Cited by 95 publications

(140 citation statements)

References 36 publications

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“…Previous studies [21,22,27,64,65] have shown that a helical hypermagnetic field in the symmetric phase of the EW plasma sources baryon number, which thereby competes against the washout of baryon number by EW sphalerons [74]. Unlike the earlier work, in Sec.…”

Section: Analytic Equilibrium Solutionmentioning

confidence: 80%

“…These ideas were formulated into a model of baryogenesis by Bamba [25] where the dynamics of an axion field during inflation leads to the growth of a helical hypermagnetic field with a large correlation length, which is partially converted into baryon number by the SM anomalies at the electroweak phase transition (see also Refs. [26,27]). Other related work has explored the connection between helical magnetic fields in the early Universe and the anomalous violation of chiral charge [28][29][30][31][32] (see also Refs.…”

Section: Introductionmentioning

confidence: 99%

“…In the early works of Giovannini and Shaposhnikov and Bamba, et al [21][22][23][24][25][26] it was argued that the EW phase transition must be first order so that the EW sphaleron process is out of equilibrium in the broken phase and washout of baryon number is avoided. The assumption is implicit in later work [27,64] where baryon-number violation due to both the EW sphaleron and the hypermagnetic field are assumed to shut off simultaneously at EW temperatures. [65] recently demonstrated that a complete washout of baryon number is avoided even if there is no B − L asymmetry and the EW phase transition is a continuous crossover as we expect in the SM.…”

Section: Introductionmentioning

confidence: 99%

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Evolution of the baryon asymmetry through the electroweak crossover in the presence of a helical magnetic field

2016

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We elaborate upon the model of baryogenesis from decaying magnetic helicity by focusing on the evolution of the baryon number and magnetic field through the Standard Model electroweak crossover. The baryon asymmetry is determined by a competition between the helical hypermagnetic field, which sources baryon number, and the electroweak sphaleron, which tends to wash out baryon number. At the electroweak crossover both of these processes become inactive; the hypermagnetic field is converted into an electromagnetic field, which does not source baryon number, and the weak gauge boson masses grow, suppressing the electroweak sphaleron reaction. An accurate prediction of the relic baryon asymmetry requires a careful treatment of the crossover. We extend our previous study [K. Kamada and A. J. Long, Phys. Rev. D 94, 065301 (2016)], taking into account the gradual conversion of the hypermagnetic into the electromagnetic field. If the conversion is not completed by the time of sphaleron freeze-out, as both analytic and numerical studies suggest, the relic baryon asymmetry is enhanced compared to previous calculations. The observed baryon asymmetry of the Universe can be obtained for a primordial magnetic field that has a present-day field strength and coherence length of B 0 ∼ 10 −17 G and λ 0 ∼ 10 −3 pc and a positive helicity. For larger B 0 the baryon asymmetry is overproduced, which may be in conflict with blazar observations that provide evidence for an intergalactic magnetic field of strength B 0 10

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Section: Analytic Equilibrium Solutionmentioning

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Evolution of the baryon asymmetry through the electroweak crossover in the presence of a helical magnetic field

2016

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“…Depending on the form of the coupling f , this gives rise to different magnetic field power spectra [31,[36][37][38][39][40][41]. Alternative models, in which magnetogenesis is driven by a rolling pseudo-Goldstone boson ϕ through its coupling to the electromagnetic field in the form ϕFF , are also very interesting and much studied [42][43][44][45][46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Magnetogenesis during inflation and preheating in the Starobinsky model

et al. 2017

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By assuming the kinetic coupling f 2 (φ)F F of the effective inflaton field φ with the electromagnetic field, we explore magnetogenesis during the inflation and preheating stages in the R 2 Starobinsky model [1]. We consider the case of the exponential coupling function f (φ) = exp(αφ/Mp) and show that for α ∼ 12 − 15 it is possible to generate the large scale magnetic fields with strength 10 −15 Gauss at the present epoch. The spectrum of generated magnetic fields is blue with the spectral index n = 1+s, s > 0. We have found that for the relevant values of the coupling parameter, α = 12 − 15, model avoids the back-reaction problem for all relevant modes.

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“…Therefore, most of the scenarios presented for the generation of the seed fields in the early Universe operate either at a phase transition [28][29][30][31][32][33][34] or during the inflation [35][36][37][38][39][40][41]. The inflationary mechanisms have received a lot of attention, since they have the advantage of achieving super-horizon correlations and therefore generate much more coherent magnetic fields in the early Universe.…”

Section: Introductionmentioning

confidence: 99%

Effects of theUY(1)Chern-Simons term and its baryonic contribution on matter asymmetries and hypermagnetic fields

Zadeh

Gousheh

2017

Phys. Rev. D

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In this paper, we study the significance of the U Y (1) Chern-Simons term in general, and its baryonic contribution in particular, for the evolution of the matter asymmetries and the hypermagnetic field in the temperature range 100GeV≤ T ≤ 10TeV. We show that an initial helical hypermagnetic field, denoted by B (0) Y , can grow matter asymmetries from zero initial value. However, the growth which is initially quadratic with respect to B (0) Y , saturates for values larger than a critical value. The inclusion of the baryonic contribution reduces this critical value, leading to smaller final matter asymmetries. Meanwhile, B Y (T EW ) becomes slightly larger than B (0)Y . In the absence of the U Y (1) Chern-Simons term, the final values of matter asymmetries grow without saturation. Conversely, we show that an initial matter asymmetry can grow an initial seed of hypermagnetic field, provided the Chern-Simons term is taken into account. The growth process saturates when the matter asymmetry drops abruptly. When the baryonic contribution is included, the saturation occurs at an earlier time, and B Y (T EW ) becomes larger. We also show that the baryonic asymmetry and the magnetic field strength can be within the acceptable range of present day data, provided the inverse cascade process is also taken into account; however, the magnetic field scale obtained from this simple model is much lower than the ones usually assumed for gamma ray propagation. * S − Rostamzadeh@sbu.ac.ir † ss−gousheh@sbu.ac.ir 1 arXiv:1607.00650v3 [hep-ph]

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Hypermagnetic fields and baryon asymmetry from pseudoscalar inflation

Cited by 95 publications

References 36 publications

Evolution of the baryon asymmetry through the electroweak crossover in the presence of a helical magnetic field

Evolution of the baryon asymmetry through the electroweak crossover in the presence of a helical magnetic field

Magnetogenesis during inflation and preheating in the Starobinsky model

Effects of theUY(1)Chern-Simons term and its baryonic contribution on matter asymmetries and hypermagnetic fields

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