HR: 0830h
AN: SH21B-0134    [PDF]
TI: Evolution of Two Ion component Plasma In a Random Magnetic Field: Numerical Study
AU: Vasquez, B J
EM: bernie.vasquez@unh.edu
AF: Institute for the study of Earth, Oceans and Space, University of New Hampshire, Durham, CA 03824 United States
AU: * Kaghashvili, E K
EM: ekaghash@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, Riverside, CA 92521 United States
AU: Zank, G P
EM: zank@ucrac1.ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, Riverside, CA 92521 United States
AB: Wave spectra at frequencies near and below the proton cyclotron frequency can develop in coronal and solar wind plasmas via turbulence and nonthermal particle processes. These spectra can often be described by a decreasing power law in wave frequency (or wavenumber). Ions can cyclotron resonate with these waves and experience significant heating. Although protons are dominant in the solar wind, other species can have important effects because with their lower cyclotron frequencies they can resonate with waves of greater amplitude. We address the issue of how energy is distributed between different ion populations, particularly how much energy passes to a minor species relative to cases with only protons. We present hybrid numerical simulations with particle ions and fluid electrons of the heating of protons alone and compare this to cases with both protons and alpha particles. Wave spectra are treated as phase random fields. We consider a range of relative alpha number densities, temperatures, and streaming speeds as well as different power law spectra.
DE: 2164 Solar wind plasma
DE: 7843 Numerical simulation studies
DE: 7867 Wave/particle interactions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting