A model of nonlinear evolution and saturation of the turbulent MHD dynamo by Schekochihin, A, Cowley, S, Hammett, G, Maron, J, McWilliams, J

“…This regime is very common in low-density hot astrophysical plasmas. During the early (kinematic) stage, weak magnetic fluctuations grow exponentially and concentrate at the resistive scale, which lies far below the hydrodynamic viscous scale. …”

A model of nonlinear evolution and saturation of the turbulent MHD dynamo by Schekochihin, A, Cowley, S, Hammett, G, Maron, J, McWilliams, J

“…This regime is very common in low-density hot astrophysical plasmas. During the early (kinematic) stage, weak magnetic fluctuations grow exponentially and concentrate at the resistive scale, which lies far below the hydrodynamic viscous scale. …”

Simulations of the small-scale turbulent dynamo by Schekochihin, A, Cowley, S, Taylor, S, Maron, J, McWilliams, J

“…The primary focus is on the case of large magnetic Prandtl numbers Prm, which is relevant for hot low-density astrophysical plasmas. A Prm parameter scan is given for the model case of viscosity-dominated (low Reynolds number) turbulence. …”