Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh21a0728v&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH21A-0728
Physics
2149 Mhd Waves And Turbulence, 2164 Solar Wind Plasma
Scientific paper
We present hybrid simulations of wave-particle interactions in the solar wind, including the effects of the mirror force on the proton and alpha-particle distribution functions. In previous work, we showed how hybrid simulations using the expanding box model were able to describe particle distribution deformation due to wave absorption including important phenomena such as frequency streaming of the wave-spectrum due to the decay of Alfvén speed with distance from the sun (Liewer, P.C., Velli, M. and Goldstein, B.E., JGR 2001 in press). In its original formulation, gradients of a background radial or spiral magnetic field within the box were neglected, and the global heliospheric magnetic field was taken to be uniform at the box scale, with a time variability due to the motion of the plasma. In the supersonic region of the wind, we assumed the mirror force to be negligible, or rather, we assume the mirror force to only contribute in defining the asymptotic wind speed. However, the non-vanishing radial gradient of the magnetic field will cause a force, within the box, which tends to distort distribution functions. This force is uniform in space (at the scale of the box), time-dependent via the decreasing magnetic field with distance, and tends to accelerate particles with a larger than average perpendicular temperature, and decelerate particles with a cooler than average perpendicular temperature. This term significantly improves the description of particle behaviour in our model, especially close to the sun, as the mirror force will provide a secular deformation of distribution functions, consistent with their radial streaming from the sun, even in the absence of waves. Our new simulations will be compared to previous results as well as semi-analytical kinetic models of the solar wind.
Goldstein Bruce E.
Liewer Paulett C.
Velli M. M.
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