Chromospheric and coronal Alfvenic oscillations in non-vertical magnetic fields

Details Chromospheric and coronal Alfvenic oscillations in non-vertical magnetic fields Chromospheric and coronal Alfvenic oscillations in non-vertical magnetic fields

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...92...81s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 92, May 1984, p. 81-98. Research supported by the Nuffield Foundation and Science and Engin

Physics

30

Chromosphere, Plasma Oscillations, Solar Corona, Solar Magnetic Field, Solar Physics, Atmospheric Stratification, Energy Transfer, Frequency Response, Inhomogeneity, Magnetic Field Configurations

Scientific paper

Previous studies of Alfvenic oscillations in the solar atmosphere are generalized to geometries in which the background magnetic field is not parallel to the gravitational acceleration. A uniform but inclined field produces only subtle changes in the mathematics, and virtually no changes to the coronal energy flux, over previous vertical field studies. It is shown that simple, two-layer models agree remarkably well with more sophisticated, multi-layer calculations. In addition, several useful and accurate analytic results are derived which highlight many features and parameter dependences. A model with a spreading field geometry is also studied. For low magnetic fields (about 10 G) the corona still appears WKB to the oscillations and no significant deviations from the uniform field calculations are found. This is not the case for higher magnetic fields in active regions (about 3000 G) where previous results which suggest an order of magnitude increase in the coronal flux are confirmed. Again, useful analytic approximations are derived.

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