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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7472
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dc.contributor.authorGupta, Siddhartha-
dc.contributor.authorNath, Biman B.-
dc.contributor.authorSharma, Prateek-
dc.contributor.authorEichler, D.-
dc.date.accessioned2020-05-27T06:47:24Z-
dc.date.available2020-05-27T06:47:24Z-
dc.date.issued2020-04-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2020, Vol.493, p3159–3177en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/7472-
dc.descriptionOpen Accessen_US
dc.description.abstractCosmic ray (CR) sources leave signatures in the isotopic abundances of CRs. Current models of Galactic CRs that consider supernovae (SNe) shocks as the main sites of particle acceleration cannot satisfactorily explain the higher 22Ne/20Ne ratio in CRs compared to the interstellar medium. Although stellar winds from massive stars have been invoked, their contribution relative to SNe ejecta has been taken as a free parameter. Here, we present a theoretical calculation of the relative contributions of wind termination shocks (WTSs) and SNe shocks in superbubbles, based on the hydrodynamics of winds in clusters, the standard stellar mass function, and stellar evolution theory. We find that the contribution of WTSs towards the total CR production is at least 25{{ per cent}}, which rises to ≳ 50{{ per cent}} for young (≲10 Myr) clusters, and explains the observed 22Ne/20Ne ratio. We argue that since the progenitors of apparently isolated supernovae remnants (SNRs) are born in massive star clusters, both WTS and SNe shocks can be integrated into a combined scenario of CRs being accelerated in massive clusters. This scenario is consistent with the observed ratio of SNRs to γ-ray bright (Lγ ≳ 1035 erg s-1) star clusters, as predicted by star cluster mass function. Moreover, WTSs can accelerate CRs to PeV energies, and solve other long-standing problems of the standard SN paradigm of CR acceleration.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/2020MNRAS.493.3159G/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1910.10168en_US
dc.relation.urihttps://doi.org/10.1093/mnras/staa286en_US
dc.rights2020 The Author(s)en_US
dc.subjecthydrodynamics – shock waves – methodsen_US
dc.subjectnumerical – cosmic raysen_US
dc.titleRealistic modelling of wind and supernovae shocks in star clusters: addressing 22Ne/20Ne and other problems in Galactic cosmic raysen_US
dc.typeArticleen_US
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