Proton Perpendicular Heating in Association With a Velocity Shear Instability

Details Proton Perpendicular Heating in Association With a Velocity Shear Instability Proton Perpendicular Heating in Association With a Velocity Shear Instability

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh43a..14v&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH43A-14

Physics

2149 Mhd Waves And Turbulence, 2164 Solar Wind Plasma, 7843 Numerical Simulation Studies, 7867 Wave/Particle Interactions, 7871 Waves And Instabilities

Scientific paper

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.

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