Nonlinear Alpha Effect in Dynamo Theory

Abstract

We extend the standard two-scale theory of the turbulent dynamo coefficient $α$ to include the nonlinear back reaction of the mean field $\bar B$ on the turbulence. We calculate the turbulent emf as a power series in $\bar B$, assuming that the base state of the turbulence ($\bar B=0$) is isotropic, and, for simplicity, that the magnetic diffusivity equals the kinematic viscosity. The power series converges for all $\bar B$, and for the special case that the spectrum of the turbulence is sharply peaked in $k$, our result is proportional to a tabulated function of the magnetic Reynolds number $R_M$ and the ratio $β$ of $\bar B$ (in velocity units) to the rms turbulent velocity $v_0$. For $β\to 0$ (linear regime) we recover the results of Steenbeck et al. (1966) as modified by Pouquet et al. (1976). For $R_M\gg 1$, the usual astrophysical case, $α$ starts to decrease at $β\sim 1$, dropping like $β^{-2}$ as $β\to \infty$. Hence for large $R_M$, $α$ saturates at $\bar B\sim v_0$, as estimated by Kraichnan (1979), rather than at $\bar B\sim R^{-1/2}_Mv_0$, as inferred by Cattaneo and Hughes (1996) from their numerical simulations at $R_M$=100. We plan to carry out simulations with various values of $R_M$ to investigate the discrepency.