Other
Scientific paper
Apr 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..644s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, April 1, 1992, p. 644-647.
Other
15
Magnetohydrodynamic Waves, Solar Atmosphere, Solar Magnetic Field, Wave Propagation, Wave Reflection, Magnetic Field Configurations, Magnetic Flux, Photosphere, Solar Corona
Scientific paper
The transmission and reflection coefficients of shear Alfven waves in an open magnetic structure emerging from the sun are determined. Both 2D slab and axisymmetric static equilibrium configurations are solved numerically on a curvilinear coordinate grid adapted to the magnetic field geometry and to the density stratification. The equilibrium structure obtained numerically extends from the photosphere up to an altitude of 20,000 km, spanning 14 density scale heights and allowing for a magnetic flux tube expansion by a factor 40-400, corresponding to a filling factor of 2.5 to 0.25 percent. From 20,000 km up to 4 solar radii a magnetic monopole model is adopted. The Alfven wave equation is solved for wave periods ranging from 10 s to 10,000 s for which the WKB approximation is not valid. It is shown that because of magnetic expansion the coefficient of transmission of Alfven waves from the photosphere to 4 solar radii has values about 5-30 percent for wave periods in the minutes range. Thus magnetic expansion allows a significant Alfven energy flux to propagate from photosphere to corona, an effect especially important for open magnetic structures where other heating mechanisms such as nanoflares are not operative.
Similon Philippe L.
Zargham Shahrokh
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