Modeling the Preferential Acceleration and Heating of Coronal Hole O5+ as Measured by UVCS/SOHO

Details Modeling the Preferential Acceleration and Heating of Coronal Hole O5+ as Measured by UVCS/SOHO Modeling the Preferential Acceleration and Heating of Coronal Hole O5+ as Measured by UVCS/SOHO

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216...56i&link_type=abstract

TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 56-59 (2010).

Physics

1

Solar Wind, Cyclotron Resonance, Electric Fields, Magnetic Field Effects, Particle Emission, Solar Wind, Plasma Heating By Radio-Frequency Fields, Icr, Icp, Helicons, Electric Fields, Field-Aligned Currents And Current Systems, And Ring Currents, Electric And Magnetic Fields, Solar Magnetism

Scientific paper

We have recently presented a mechanism for preferential acceleration and heating of coronal hole minor ions [1, 2]. The energization is due to the effect of multiple cyclotron resonances in the presence of sunward and anti-sunward dispersive ion cyclotron waves, providing a second-order Fermi interaction. The mechanism is preferential because coronal hole protons do not experience such multiple resonances. The detailed model results depend on many parameters, including poorly-known quantities such as the wave intensities, spectral shapes and radial profiles. In this paper, we show that reasonable choices for these quantities can yield excellent agreement with the observations. We find that only a small fraction of the extrapolated wave power is needed to provide the observed heating, and there is an indication that the resonant wave levels are increasing with radial position between r = 2 Rs and 4 Rs.

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