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We discuss processes in galactic cosmic ray (GCR) acceleration sites -supernova remnants, compact associations of young massive stars, andsuperbubbles. Mechanisms of efficient conversion of the mechanical power of theoutflows driven by supernova shocks and fast stellar winds of young stars intomagnetic fields and relativistic particles are discussed. The high efficiencyof particle acceleration in the sources implies the importance of nonlinearfeedback effects in a symbiotic relationship where the magnetic turbulencerequired to accelerate the CRs is created by the accelerated CRs themselves.Non-thermal emission produced by relativistic particles (both those confined inand those that escape from the cosmic accelerators) can be used to constrainthe basic physical models of the GCR sources. High resolution X-ray synchrotronimaging, combined with GeV-TeV gamma ray spectra, is a powerful tool to probethe maximum energies of accelerated particles. Future MeV regime spectroscopywill provide unique information on the composition of accelerated particles.

Galactic Cosmic Ray Origin Sites: Supernova Remnants and Superbubbles