Magnetic field generation from PBH distributions

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dc.contributor.authorAraya, I. J.
dc.contributor.authorRubio, M. E.
dc.contributor.authorSan Martin, M.
dc.contributor.authorStasyszyn, F. A.
dc.contributor.authorPadilla, N. D.
dc.contributor.authorMagana, J.
dc.contributor.authorSureda, J.
dc.date.accessioned2025-01-20T23:51:49Z
dc.date.available2025-01-20T23:51:49Z
dc.date.issued2021
dc.description.abstractWe introduce a statistical method for estimating magnetic field fluctuations generated from primordial black hole (PBH) populations. To that end, we consider monochromatic and extended Press-Schechter PBH mass functions, such that each constituent is capable of producing its own magnetic field due to some given physical mechanism. Assuming a linear correlation between magnetic field fluctuations and matter overdensities, our estimates depend on the mass function, the physical field generation mechanism by each PBH constituent, and the characteristic PBH separation. After computing the power spectrum of magnetic field fluctuations, we apply our formalism to study the plausibility that two particular field generation mechanisms could have given rise to the expected seed fields according to current observational constraints. The first mechanism is the Biermann battery and the second one is due to the accretion of magnetic monopoles at PBH formation, constituting magnetic PBHs. Our results show that, for monochromatic distributions, it does not seem to be possible to generate sufficiently intense seed fields in any of the two field generation mechanisms. For extended distributions, it is also not possible to generate the required seed field by only assuming a Biermann battery mechanism. In fact, we report an average seed field by this mechanism of about 10(-47) G, at z = 20. For the case of magnetic monopoles, we instead assume that the seed values from the literature are achieved and calculate the necessary number density of monopoles. In this case, we obtain values that are below the upper limits from current constraints.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stab729
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stab729
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94861
dc.identifier.wosidWOS:000649000600090
dc.issue.numero3
dc.language.isoen
dc.pagina.final4399
dc.pagina.inicio4387
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectMagnetic Fields
dc.subjectDark Matter
dc.subjectBlack Hole Physics
dc.titleMagnetic field generation from PBH distributions
dc.typeartículo
dc.volumen503
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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