HR: 0800h
AN: SH51A-1195    [Abstracts]
TI: Non-linear Energetic Particle Transport in Incompressible MHD Turbulence
AU: Verkhoglyadova, O P
EM: olgav@citrus.ucr.edu
AF: University of California, 900 University Avenue, Riverside, CA 92521 United States
AU: * le Roux, J A
EM: jakobus.leroux@ucr.edu
AF: University of California, 900 University Avenue, Riverside, CA 92521 United States
AU: Webb, G M
EM: gmwebb@ucr.edu
AF: University of California, 900 University Avenue, Riverside, CA 92521 United States
AB: We investigate theoretically non-linear energetic particle diffusive transport in MHD solar wind turbulence assumed to be mainly composed of incompressible 2D turbulence and 1D parallel-propagating Alfven waves. Different from the Taylor-Green-Kubo formalism, where only the diffusion coefficients themselves are calculated, we start the derivation with a BGK-Boltzmann equation where the full energetic particle transport equation including the expressions of the diffusion tensor can be derived. The theory is non-linear in the sense that particle orbits are randomized on a turbulence correlation scale by the BGK scattering term representing a model for orbit distortion. This general formalism allows one to derive the full diffusion tensor (parallel diffusion, perpendicular diffusion and gradient and curvature drifts) for particle transport interacting with relatively large-scale random 2D turbulence and Alfven waves, and to take different limits such as: (i) the standard quasi-linear limit where particle orbits are undisturbed on a correlation scale which could be appropriate for the quiet solar wind, (ii) a different quasi-linear limit where small-scale MHD turbulence distorts the particle orbits on a correlation scale but the large-scale turbulence is too weak to affect the particle orbits, which is perhaps applicable upstream of turbulent shocks where the small-scale turbulence is enhanced by wave generation from particles streaming away from the shock and, (iii) the non-linear limit where both the large-scale and small-scale MHD turbulence affect the particle orbits on a correlation scale which could be useful downstream of shocks where turbulence at all scales are enhanced.
DE: 2104 Cosmic rays
DE: 2149 MHD waves and turbulence (2752, 6050, 7836)
DE: 7827 Kinetic and MHD theory
DE: 7859 Transport processes
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005