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.
The exceptionally powerful TeV gamma-ray emitters in the Large Magellanic Cloud
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abstract
The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known N 157B, the radio-loud supernova remnant N 132D and the largest non-thermal X-ray shell - the superbubble 30 Dor C. The unique object SN 1987A is, surprisingly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a gamma-ray source population in an external galaxy, and provide via 30 Dor C the unambiguous detection of gamma-ray emission from a superbubble.
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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.