The limited contribution of low- and high-luminosity gamma-ray bursts to ultra-high-energy cosmic rays

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dc.contributor.authorSamuelsson, Filip
dc.contributor.authorBégué, Damien
dc.contributor.authorRyde, Felix
dc.contributor.authorPe’er, Asaf
dc.contributor.funderSwedish National Space Agencyen
dc.contributor.funderSvenska Forskningsrådet Formasen
dc.contributor.funderDeutsche Forschungsgemeinschaften
dc.contributor.funderGöran Gustafssons Stiftelse för Naturvetenskaplig och Medicinsk Forskningen
dc.contributor.funderEuropean Research Councilen
dc.date.accessioned2019-09-10T16:03:50Z
dc.date.available2019-09-10T16:03:50Z
dc.date.issued2019-05-08
dc.description.abstractThe acceleration site for ultra-high-energy cosmic rays (UHECRs) is still an open question despite extended research. In this paper, we reconsider the prompt phase of gamma-ray bursts (GRBs) as a possible candidate for this acceleration and constrain the maximum proton energy in optically thin synchrotron and photospheric models, using properties of the prompt photon spectra. We find that neither of the models favors acceleration of protons to 1020 eV in high-luminosity bursts. We repeat the calculations for low-luminosity GRBs (llGRBs) considering both protons and completely stripped iron and find that the highest obtainable energies are <1019 eV and <1020 eV for protons and iron respectively, regardless of the model. We conclude therefore that for our fiducial parameters, GRBs, including low-luminosity bursts, contribute little to nothing to the UHECRs observed. We further constrain the conditions necessary for an association between UHECRs and llGRBs and find that iron can be accelerated to 1020 eV in photospheric models, given very efficient acceleration and/or a small fractional energy given to a small fraction of accelerated electrons. This will necessarily result in high prompt optical fluxes, and the detection of such a signal could therefore be an indication of successful UHECR acceleration at the source.en
dc.description.sponsorshipSwedish National Space Agency (196/16); Swedish Research Council (Vetenskapsrådet, 2018-03513); Deutsche Forschungsgemeinschaft (SFB 1258).en
dc.description.statusPeer revieweden
dc.description.versionPublished Versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.articleid93en
dc.identifier.citationSamuelsson, F., Bégué, D., Ryde, F. and Pe’er, A. (2019) 'The Limited Contribution of Low- and High-luminosity Gamma-Ray Bursts to Ultra-high-energy Cosmic Rays', The Astrophysical Journal, 876(2), 93. (17pp.) DOI: 10.3847/1538-4357/ab153cen
dc.identifier.doi10.3847/1538-4357/ab153cen
dc.identifier.eissn1538-4357
dc.identifier.endpage17en
dc.identifier.issn0004-637X
dc.identifier.issued2en
dc.identifier.journaltitleAstrophysical Journalen
dc.identifier.startpage1en
dc.identifier.urihttps://hdl.handle.net/10468/8509
dc.identifier.volume876en
dc.language.isoenen
dc.publisherInstitute of Physics Publishingen
dc.relation.projectinfo:eu-repo/grantAgreement/EC/H2020::ERC::ERC-COG/773062/EU/Origin and Magnetization of astronomical Jets/O.M.J.en
dc.relation.urihttps://iopscience.iop.org/article/10.3847/1538-4357/ab153c
dc.rights©2019. The American Astronomical Society. All rights reserveden
dc.subjectGamma-ray bursten
dc.subjectGeneralen
dc.subjectCosmic raysen
dc.titleThe limited contribution of low- and high-luminosity gamma-ray bursts to ultra-high-energy cosmic raysen
dc.typeArticle (peer-reviewed)en
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