Broadening of solar wind strahl pitch-angles by the electron/electron instability: Particle-in-cell simulations

Details Broadening of solar wind strahl pitch-angles by the electron/electron instability: Particle-in-cell simulations Broadening of solar wind strahl pitch-angles by the electron/electron instability: Particle-in-cell simulations

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007georl..3414111g&link_type=abstract

Geophysical Research Letters, Volume 34, Issue 14, CiteID L14111

Physics

Plasma Physics

8

Interplanetary Physics: Plasma Waves And Turbulence, Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Kinetic Waves And Instabilities, Space Plasma Physics: Nonlinear Phenomena (4400, 6944), Space Plasma Physics: Wave/Particle Interactions (2483, 6984)

Scientific paper

Solar wind electrons in the suprathermal energy range from about 70 eV to greater than 1 keV usually are observed as two distinct, relatively tenuous components: an approximately isotropic halo and a strongly anisotropic ``strahl'' directed along the magnetic field. This manuscript describes a two-dimensional electromagnetic particle-in-cell simulation in a magnetized, homogeneous, collisionless plasma with such a two-component representation of suprathermal electrons. In this computation the electrostatic electron/electron instability is driven by a strahl with a large average speed along the background magnetic field B o . The simulation demonstrates that this instability leads to substantial strahl velocity scattering perpendicular to B o . The most important result here is that, for strahl speeds large compared to the halo thermal speed, after instability saturation the width of the electron pitch-angle distribution exhibits a maximum as a function of electron energy.

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