Spectroscopic Constraints on Models of Ion-Cyclotron Resonance Heating in the Polar Solar Corona and Fast Solar Wind

Details Spectroscopic Constraints on Models of Ion-Cyclotron Resonance Heating in the Polar Solar Corona and Fast Solar Wind Spectroscopic Constraints on Models of Ion-Cyclotron Resonance Heating in the Polar Solar Corona and Fast Solar Wind

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998eostr..79..722c&link_type=abstract

Eos Trans. AGU, 79 (45), Fall Meeting Suppl., F722 (SH42A-10)

Astronomy and Astrophysics

Astrophysics

Solar Corona, Solar Wind, Alfven Waves, Ion Cyclotron Resonance, Mhd Wave Damping, Uvcs, Sumer, Soho

Scientific paper

We present preliminary results from a theoretical model of the heating of minor ions in the fast solar wind. We examine the compatibility between these models and spectroscopic determinations of velocity distribution functions from the UVCS and SUMER instruments aboard SOHO. By examining the dependence of line shapes (which probe the perpendicular velocity distribution) on ion charge and mass, detailed information can be extracted about the preferential heating and the Coulomb collisional coupling. The primary momentum and energy deposition mechanism we investigate is the dissipation of high-frequency (ion-cyclotron resonant) Alfven waves, which can accelerate and heat ions differently depending on their charge and mass. Minor ions which do not appreciably damp the resonant wave amplitudes can be used to constrain the slope of the fluctuation spectrum. SUMER measurements of several ions at heliocentric heights between 1.02 and 1.07 solar radii allow the ``base'' spectrum to be analyzed, and UVCS O VI line widths measured between 1.5 and 3.5 solar radii provide information about the radial evolution of the spectrum. This work is supported by the National Aeronautics and Space Administration under grant NAG5-3192 to the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana, and by the ESA PRODEX program (Swiss contribution).

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