3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
Monthly Notices of the Royal Astronomical Society , archivePrefix = "arXiv", eprint =
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Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.
citing papers explorer
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Direct simulations of very high energy cosmic ray acceleration in 3D MHD model of a compact star cluster
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
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Diffuse gamma-ray emissions around the stellar cluster Berkeley 59
Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.