Speaker
Description
Supernova remnants and pulsar wind nebulae are likely sources of Galactic cosmic-ray protons and electrons, but these are not sufficient; these sources are generally unable to explain cosmic rays with energies of ~1 PeV. To explain cosmic rays with PeV energies requires sources to accelerate them to these energies, so-called PeVatrons. These cosmic-ray PeVatrons must accelerate protons (hadrons) but likely also accelerate electrons (leptons). Gamma-ray observatories have detected gamma-ray emission above 100 TeV from over a few dozen sources, marking them as PeVatron candidates. The question remains whether or not the emission is primarily hadronic or leptonic. I will present a framework for leptonic modeling of ultra-high-energy gamma-ray sources which retains spectral and spatial information. I then apply this framework to LHAASO observations of SS 433 and H.E.S.S. observation of the Galactic center.