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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7200
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dc.contributor.authorJana, Ranita-
dc.contributor.authorNath, Biman B.-
dc.contributor.authorBiermann, Peter L.-
dc.date.accessioned2019-05-03T18:25:06Z-
dc.date.available2019-05-03T18:25:06Z-
dc.date.issued2019-03-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2019, Vol.483, p 5329–5333en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 - (online)-
dc.identifier.urihttp://hdl.handle.net/2289/7200-
dc.descriptionOpen Access.en_US
dc.description.abstractWe consider the synchrotron emission from high-energy electrons accelerated in supernova explosions of massive Population III stars in high-redshift minihaloes of mass 105−7M⊙⁠. We show the resulting intensity of radio background from this process can be substantial, which could potentially explain the recently reported EDGES result, if not for the associated heating of the IGM by CR protons, which are also produced at the same time. The trade-off between the radio background and heating is such that the 21 cm brightness temperature cannot be larger than |ΔT21| ∼ 0.25 K. The radio background and heating are both produced by energetic particles, although one by energetic electrons and the other by energetic protons. The two competing processes, production of radio background and heating of IGM by Pop III supernovae, determine the depth of the trough in the 21 cm brightness temperature, which can be observed in future experiments and used as a test of this scenario.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2019MNRAS.483.5329J/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1812.07404en_US
dc.relation.urihttps://doi.org/10.1093/mnras/sty3426en_US
dc.rights2019 The Author(s)en_US
dc.subjectsupernovae: generalen_US
dc.subjectcosmic raysen_US
dc.subjectintergalactic mediumen_US
dc.subjectdark agesen_US
dc.subjectfirst starsen_US
dc.subjectreionizationen_US
dc.titleRadio background and IGM heating due to Pop III supernova explosionsen_US
dc.typeArticleen_US
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