Cosmological magnetic fields: their generation, evolution and observation

Durrer, Ruth; Neronov, A.

doi:10.1007/s00159-013-0062-7

Cited by 758 publications

(1,084 citation statements)

References 291 publications

(475 reference statements)

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“…4. Nevertheless, one should bear in mind that the current upper limits of coherence length of magnetic fields in voids range between a few and hundreds of Mpc [57], placing the chosen value of 120 Mpc well within the allowed bounds.…”

Section: Discussion and Outlookmentioning

confidence: 91%

Probing intergalactic magnetic fields with simulations of electromagnetic cascades

et al. 2016

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We determine the effect of intergalactic magnetic fields on the distribution of high energy gamma rays by performing three-dimensional Monte Carlo simulations of the development of gamma-rayinduced electromagnetic cascades in the magnetized intergalactic medium. We employ the so-called "Large Sphere Observer" method to efficiently simulate blazar gamma ray halos. We study magnetic fields with a Batchelor spectrum and with maximal left-and right-handed helicities. We also consider the case of sources whose jets are tilted with respect to the line of sight. We verify the formation of extended gamma ray halos around the source direction, and observe spiral-like patterns if the magnetic field is helical. We apply the Q-statistics to the simulated halos to extract their spiral nature and also propose an alternative method, the S-statistics. Both methods provide a quantative way to infer the helicity of the intervening magnetic fields from the morphology of individual blazar halos for magnetic field strengths B 10 −15 G and magnetic coherence lengths Lc 100 Mpc. We show that the S-statistics has a better performance than the Q-statistics when assessing magnetic helicity from the simulated halos.

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Section: Discussion and Outlookmentioning

confidence: 91%

Probing intergalactic magnetic fields with simulations of electromagnetic cascades

et al. 2016

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“…[56,57]) and more detailed work will be required to verify the claim, however we already see from the plot that the Schwinger effect severely constrains the inflationary magnetogenesis scenario from producing such large-scale magnetic fields; the blue solid line shows an upper bound of |B 0 | 10 −30 G on Mpc scale and beyond. For other observational constraints on magnetic fields, see the review [58].…”

mentioning

confidence: 99%

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Kobayashi

Afshordi

2014

J. High Energ. Phys.

145

229

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We investigate pair creation by an electric field in four-dimensional de Sitter space. The expectation value of the induced current is computed, using the method of adiabatic regularization. Under strong electric fields the behavior of the current is similar to that in flat space, while under weak electric fields the current becomes inversely proportional to the mass squared of the charged field. Thus we find that the de Sitter space obtains a large conductivity under weak electric fields in the presence of a charged field with a tiny mass. We then apply the results to constrain electromagnetic fields in the early universe. In particular, we study cosmological scenarios for generating large-scale magnetic fields during the inflationary era. Electric fields generated along with the magnetic fields can induce sufficiently large conductivity to terminate the phase of magnetogenesis. For inflationary magnetogenesis models with a modified Maxwell kinetic term, the generated magnetic fields cannot exceed 10 −30 G on Mpc scales in the present epoch, when a charged field carrying an elementary charge with mass of order the Hubble scale or smaller exists in the Lagrangian. Similar constraints from the Schwinger effect apply for other magnetogenesis mechanisms.

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“…Current theoretical and observational constraints on the IGMF are summarized in the review [16]. The IGMF strength is more than about 10 −17 G and less than about 10 −9 G. As it is shown in Ref.…”

Section: Methodsmentioning

confidence: 87%

Simulations of Ultra High Energy Cosmic Rays Propagation

Kido¹

2016

Proceedings of International Symposium for Ultra-High Energy Cosmic Rays (UHECR2014)

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We fitted a pure proton source model to the spectrum of ultra-high-energy cosmic rays (UHECRs) with energy E > 10 18.2 eV based on the first six years of the surface detectors of the Telescope Array experiment. For the pure proton source model, propagation of UHECRs in inter-galactic space from uniformly distributed proton sources is simulated using the numerical code TransportCR. In the fitting, the index of the power law injection energy spectrum, the evolution of the source density with redshift, the shift of the energy scale and the normalization of the flux are considered as free parameters. We obtained satisfactory fit results assuming strong evolution of the source density. We also discuss preliminary constraints on the free parameters.

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Cosmological magnetic fields: their generation, evolution and observation

Cited by 758 publications

References 291 publications

Probing intergalactic magnetic fields with simulations of electromagnetic cascades

Probing intergalactic magnetic fields with simulations of electromagnetic cascades

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Simulations of Ultra High Energy Cosmic Rays Propagation

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