Physics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0112m&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0112
Physics
2169 Sources Of The Solar Wind, 7511 Coronal Holes, 7827 Kinetic And Mhd Theory, 7867 Wave/Particle Interactions
Scientific paper
Recently, we suggested [Hollweg and Markovskii, JGR, 107, No. 6, 2002; Markovskii and Hollweg, GRL, 29, No. 17, 2002] that the source of ion heating in coronal holes is small-scale reconnection events (microflares) at the coronal base. The microflares launch intermittent heat flux up into the corona exciting ion cyclotron waves through a plasma microinstability. The ions are heated by these waves during the microflare bursts and then evolve with no energy input between the bursts. We show that the structure of the proton distribution in the relatively long time periods between the microflares is determined by collisions at small heliocentric distances. At greater distances, the collisional processes are replaced by similar processes due to secondary instabilities. These are excited by the distortion of the distribution under the action of the mirror force. At the same time, the heating during the microflare bursts is not considerably affected either by the collisions or by the secondary instabilities, because of the short duration of the bursts. The overall coronal heating by this mechanism is a summed effect of all microflare bursts during the expansion time of the solar wind and adiabatic cooling between the microflares. Our calculations for the collision-dominated region suggest that the overall heating is efficient enough to account for the acceleration of the fast solar wind in this region. Further development of the model including the collisionless region will be reported elsewhere.
Hollweg Joseph V.
Markovskii Sergei A.
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