HR: 1330h
AN: SH43A-14    [Abstracts]
TI: Proton Perpendicular Heating in Association With a Velocity Shear Instability
AU: * Vasquez, B J
EM: bernie.vasquez@unh.edu
AF: University of New Hampshire, Space Science Center, Durham, NH 03824 United States
AU: Markovskii, S A
EM: sergei.markovskii@unh.edu
AF: University of New Hampshire, Space Science Center, Durham, NH 03824 United States
AU: Smith, C W
EM: Charles.Smith@unh.edu
AF: University of New Hampshire, Space Science Center, Durham, NH 03824 United States
AB: We examine how a velocity shear instability excites waves at proton cyclotron harmonics and heats the protons across the magnetic field. A hybrid simulation with particle protons and massless fluid electrons is employed. From the simulation results, we have obtained the proton perpendicular heating rate as a function of β_{∥(= ratio of parallel proton to magnetic field pressure). Results will be presented for the rate between β_∥} = 0.01 and β_∥ =1. The instability has been previously examined in the electrostatic limit where β_∥ ≪ 1. Our results show that heating occurs at all values of β_∥. We discuss how this instability could influence the dissipation of quasi-2D turbulence in the solar wind and also contribute to the observed perpendicular heating of solar wind protons.
DE: 2149 MHD waves and turbulence
DE: 2164 Solar wind plasma
DE: 7843 Numerical simulation studies
DE: 7867 Wave/particle interactions
DE: 7871 Waves and instabilities
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly