Abstract
Abstract The origin of magnetic fields in the universe is an open problem. Seed magnetic fields possibly produced in early times may have survived up to the present day close to their original form, providing an untapped window to the primeval universe. The recent observations of high-energy neutrinos from the blazar TXS 0506+056 in association with an electromagnetic counterpart in a broad range of wavelengths can be used to probe intergalactic magnetic fields via the time delay between the neutrinos and gamma-rays as well as the time dependence of the gamma-ray fluxes. Using extensive three-dimensional Monte Carlo simulations, we constrain both the magnetic-field strength and, for the first time, its coherence length, considering six orders of magnitude for each.
Highlights
A long-standing problem in cosmology concerns the origin of magnetic fields in the universe
Primordial and astrophysical mechanisms lead to distinct magnetic power spectra and different coherence lengths
We are able to constrain the strength of intergalactic magnetic fields (IGMFs) using information from both messengers, gamma rays cm−2s−1]
Summary
A long-standing problem in cosmology concerns the origin of magnetic fields in the universe. Two broad classes of mechanisms to explain magnetogenesis exist. Primordial (or cosmological) mechanisms posit that global processes taking place in the early universe could give rise to seed magnetic fields. Examples of such processes are inflation and phase transitions such as the electroweak and the quantum chromodynamics phase transitions (see Durrer & Neronov 2013 for a review). Astrophysical mechanisms, on the other hand, suggest that small-scale processes during the formation of structures gave rise to magnetic fields. Primordial and astrophysical mechanisms lead to distinct magnetic power spectra and different coherence lengths
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