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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6985
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dc.contributor.authorGupta, Siddhartha-
dc.contributor.authorNath, Biman B.-
dc.contributor.authorSharma, Prateek-
dc.date.accessioned2018-08-15T17:31:28Z-
dc.date.available2018-08-15T17:31:28Z-
dc.date.issued2018-10-01-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2018, Vol. 479; p5220–5234en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 - (online)-
dc.identifier.urihttp://hdl.handle.net/2289/6985-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractWe use 1D and 3D two-fluid cosmic ray (CR) hydrodynamic simulations to investigate the role of CRs in the vicinity of a compact young star cluster. We model a self-gravitating cloud (density profile ρ∝r−1), include important thermal and non-thermal processes, and explore two different CR injection scenarios. We show that if internal shocks in the wind-driving region are the main site for CR acceleration, then the resulting γ-ray luminosity (Lγ) can reach ≈5% of the mechanical luminosity (Lw), independent of the fraction of wind energy (∼1−20%) injected into CRs. In contrast, if the forward/reverse shock of a bubble is the injection site then Lγ increases linearly with the CR injection fraction, as expected analytically. We find that the X-ray luminosity (Lx) in the forward/reverse shock injection scenario is ≳10−3Lw, which is ∼10 times larger than in the central wind-driving injection case. We predict the corresponding range of the synchrotron radio luminosity. We show how multi-wavelength observations can constrain the CR parameters. Comparing the predicted multi-wavelength luminosities with those of 30 Doradus we identify the reverse shock as the most probable CR injection site, and that thermal conduction is important. We do not find significant dynamical impact of CRs in our models.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.relation.urihttps://arxiv.org/abs/1804.05877en_US
dc.relation.urihttps://arxiv.org/abs/1804.05877en_US
dc.relation.urihttps://doi.org/10.1093/mnras/sty1846en_US
dc.rights2018 The Author(s)en_US
dc.subjecthydrodynamicsen_US
dc.subjectISM: bubblesen_US
dc.subjectcosmic raysen_US
dc.subjectgalaxiesen_US
dc.subjectstar clustersen_US
dc.subjectgeneralen_US
dc.titleConstraining cosmic ray acceleration in young star clusters using multi-wavelength observationsen_US
dc.typeArticleen_US
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