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Galactic cosmic rays are thought to be accelerated at the shocks of supernova remnants via the diffusive shock acceleration mechanism. This is generally supported by observations, which via gamma-ray measurements unequivocally identify the presence of extremely relativistic particles.
Though the basic details of the process have been well-known for more than 40 years, the non-linear plasma processes that underpin the theory have only become accessible to numerical investigation in recent years. I will review the current understanding, focussing on the maximum energy
in different sources, the connection to the galactic cosmic-ray spectrum. I will conclude with some new open source tools that we are developing to study the non-linear physics of cosmic-ray acceleration
and associated plasma instabilities that facilitate the process.
Brian Reville received his PhD from University College Dublin in 2007. His thesis was on the plasma physics of magnetic field amplification at astrophysical shocks driven by energetic particle currents. He subsequently carried out postdocs at the Max-Planck Institute in Heidelberg, and at the University of Oxford, working on various aspects of astrophysical and laboratory plasma physics. In 2013 he was appointed lecturer at the Centre for Plasma Physics, at Queen's University Belfast. In 2019 he returned to Heidelberg, where he leads the Astrophysical Plasma Theory group, developing theories of relativistic particle acceleration and implications for gamma-ray astronomy.
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