Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration

Details Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.confq..66o&link_type=abstract

NASA Goddard Space Flight Center, International Solar Wind 8 Conference, p. 66

Computer Science

Solar Corona, Solar Wind, Coronal Holes, Magnetohydrodynamic Waves, Wave Propagation, Momentum, Plasma Heating, Magnetohydrodynamic Flow, Plasma Density, Plasma Resonance, Energy Dissipation, Two Dimensional Flow, Waveguides, Wavelengths, Inhomogeneity, Plasma Acceleration, Frequency Ranges, Energy Absorption

Scientific paper

Coronal hole regions are well known sources of high-speed solar wind, however to account for the observed properties of the solar wind a source of momentum and heat must be included. Alfven waves were suggested as the possible source of heating that accelerates the solar wind. We investigate the propagation of the Alfven waves in coronal holes via numerical solution of the linearized 2-D resistive MHD equations in slab geometry. The Alfven waves are driven at the lower boundary of the coronal hole and propagate into the corona. The waves are reflected at the coronal hole boundary and part of the wave energy leaks out of the coronal hole. We compare the calculated wavelengths and the attenuation rate of the fast mode Alfven waves in the leaky waveguide formed by the coronal hole with the analytical ideal MHD solutions. The formation of resonance heating layers is found to occur when shear Alfven waves propagate in an inhomogeneous coronal hole. The heating is enhanced when fast mode waves couple to the shear Alfven waves. The narrow heating layers are formed near the location of the ideal resonance, which might occur near the coronal hole boundary for a nearly constant density coronal hole, surrounded by a higher density plasma. We investigate the dependence of the heating on the driver frequency, the Lundquist number, and on the heliocentric distance. and find that the low frequency Alfven waves can be an efficient source of heating at large distances from the Sun. We discuss the relation of our results to the observed properties of high-speed solar wind and coronal holes.

Affiliated with

Also associated with

No associations

Rating

Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Heating of coronal holes by the resonant absorption and dissipation of Alfven waves and its relation to solar wind acceleration will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-760573