Propagation of waves in an atmosphere in the presence of a magnetic field. VII - Magneto-acoustic-gravity modes in an oblique B

Details Propagation of waves in an atmosphere in the presence of a magnetic field. VII - Magneto-acoustic-gravity modes in an oblique B Propagation of waves in an atmosphere in the presence of a magnetic field. VII - Magneto-acoustic-gravity modes in an oblique B

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...137..128s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 137, no. 1, Aug. 1984, p. 128-132. Research supported by the Nuffield Foundati

Physics

17

Gravity Waves, Magnetoacoustic Waves, Solar Atmosphere, Wave Propagation, Energy Transfer, Equations Of Motion, Lines Of Force, Propagation Modes, Solar Corona, Solar Magnetic Field, Solar Physics, Wave Equations

Scientific paper

The authors investigate the propagation of magneto-acoustic-gravity modes in the solar atmosphere with a magnetic field inclined at an arbitrary angle to the direction of gravity. The linearized equations of motion in this isothermally stratified atmosphere are solved via a Frobenius series method coupled with appropriate boundary conditions. Strong magnetic fields yield essentially acoustic modes propagating along the field lines and therefore suffer similar problems to previous studies. Weak magnetic fields produce a complicated competition amongst the various forces which is inefficient in transporting energy to coronal heights. Only Alfvénic motions seem to remain as a viable option for coronal heating.

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