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Beyond the Diffusion Coefficient: Propagators and Memory in Cosmic Ray Transport
Naixin Liang, S. Peng Oh
Cosmic ray (CR) transport is usually modeled with a single diffusion coefficient, but this description captures only the growth of the variance and not the full transport process.…
Cosmic Ray Drag and Damping of Compressive Turbulence
Chad Bustard, S. Peng Oh
While it is well-known that cosmic rays (CRs) can gain energy from turbulence via second order Fermi acceleration, how this energy transfer affects the turbulent cascade remains la…
Turbulent Reacceleration of Streaming Cosmic Rays
Chad Bustard, S. Peng Oh
Subsonic, compressive turbulence transfers energy to cosmic rays (CRs), a process known as non-resonant reacceleration. It is often invoked to explain observed ratios of primary to…
Fluid Simulations of Cosmic Ray Modified Shocks
Tsun Hin Navin Tsung, S. Peng Oh, Yan-Fei Jiang
We consider cosmic ray (CR) modified shocks with both streaming and diffusion in the two-fluid description. Previously, numerical codes were unable to incorporate streaming in this…
Plasma 2020 - Intracluster Medium Plasmas
Damiano Caprioli, Gianfranco Brunetti, Thomas W. Jones +6
Galaxy clusters are the largest and most massive bound objects resulting from cosmic hierarchical structure formation. Baryons account for somewhat more than 10% of that mass, with…
A New Numerical Scheme for Cosmic Ray Transport
Yan-Fei Jiang, Peng Oh
Numerical solutions of the cosmic-ray (CR) magneto-hydrodynamic equations are dogged by a powerful numerical instability, which arises from the constraint that CRs can only stream…