Acceleration and Heating of the Fast Solar Wind by Ion-Cyclotron and MHD Waves

Details Acceleration and Heating of the Fast Solar Wind by Ion-Cyclotron and MHD Waves Acceleration and Heating of the Fast Solar Wind by Ion-Cyclotron and MHD Waves

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh12a0417o&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH12A-0417

Other

7511 Coronal Holes, 7807 Charged Particle Motion And Acceleration, 7827 Kinetic And Mhd Theory, 7843 Numerical Simulation Studies, 7867 Wave/Particle Interactions

Scientific paper

The basic plasma properties of the fast solar wind as deduced from observations suggest that both, high frequency ion-cyclotron waves, and low frequency MHD waves play a role in the acceleration and heating of the coronal hole plasma. The heating due to high-frequency waves is particularly important in minor ions, such as O5+. I will present the results of 3-fluid, simulations of the solar wind plasma that combine the effects of ion-cyclotron, and MHD waves. The low frequency waves are included self-consistently as the source of momentum and heating of protons and electrons. Additional heat and momentum input terms due to ion-cyclotron waves are included in protons and minor ions. The 3-fluid gyrotropic model allows for Tperpendicular to >T_∥ of the ions in accordance with observations. The heating term that contributes mostly to the perpendicular temperature of minor ions is constructed using the saturated state of the hybrid kinetic model of the solar wind plasma at several locations in the coronal hole, with the plasma β and other parameters varying with radial distance. Iterative update of these parameters is planed in a future study. The temperature anisotropy estimated from SOHO UVCS spectral observations is used to constrain the hybrid kinetic modeling. Ulysses and Helios observations are used to constrain the asymptotic solar wind speed and mass flux.

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