Oblique Propagation and Dissipation of Alfv&én Waves in Coronal Holes

Details Oblique Propagation and Dissipation of Alfv&én Waves in Coronal Holes Oblique Propagation and Dissipation of Alfv&én Waves in Coronal Holes

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007japa...28....1s&link_type=abstract

Journal of Astrophysics & Astronomy, vol. 28, no. 1, p. 1-7

Astronomy and Astrophysics

Astrophysics

4

Sun: Alfv&Eacute, N Waves, Coronal Holes, Solar Wind.

Scientific paper

We investigate the effect of viscosity and magnetic diffusivity on the oblique propagation and dissipation of Alfvé;n waves with respect to the normal outward direction, making use of MHD equations, density, temperature and magnetic field structure in coronal holes and underlying magnetic funnels. We find reduction in the damping length scale, group velocity and energy flux density as the propagation angle of Alfvé;n waves increases inside the coronal holes. For any propagation angle, the energy flux density and damping length scale also show a decrement in the source region of the solar wind (<1.05R) where these may be one of the primary energy sources, which can convert the inflow of the solar wind into the outflow. In the outer region (>1.21R), for any propagation angle, the energy flux density peaks match with the peaks of MgX 609.78A° and 624.78A° linewidths observed from the Coronal Diagnostic Spectrometer (CDS) on SOHO and the non-thermal velocity derived from these observations, justify the observed spectroscopic signature of the Alfvén wave dissipation.

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