Speaker
Description
Cosmic ray acceleration to ~PeV energies has recently emerged as being far more common-place than previously understood. The galactic population of known “ultra high energy” (≥ 100 TeV) gamma-ray emitters encompasses a variety of source classes, including pulsar environments, stellar clusters and dark sources. At these energies, however, cosmic rays may more readily escape their accelerator and are transported into the surrounding medium. Subsequent interactions with molecular clouds may yield passive UHE sources; gamma-ray and neutrino emitters only indirectly associated with a nearby PeVatron.
In this contribution I will present examples where modelling applied to data can probe cosmic ray transport on different scales, and discuss candidate “passive” UHE sources.
