Propagation of waves in an atmosphere in the presence of a magnetic field. V - The theory of magneto-acoustic-gravity oscillations. VI - Application of magneto-acoustic-gravity mode theory to the solar atmosphere

Details Propagation of waves in an atmosphere in the presence of a magnetic field. V - The theory of magneto-acoustic-gravity oscillations. VI - Application of magneto-acoustic-gravity mode theory to the solar atmosphere Propagation of waves in an atmosphere in the presence of a magnetic field. V - The theory of magneto-acoustic-gravity oscillations. VI - Application of magneto-acoustic-gravity mode theory to the solar atmosphere

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...112...84l&link_type=abstract

Astronomy and Astrophysics, vol. 112, no. 1, Aug. 1982, p. 84-103.

Astronomy and Astrophysics

Astrophysics

44

Magnetoacoustics, Solar Atmosphere, Solar Magnetic Field, Wave Propagation, Boundary Conditions, Boundary Value Problems, Energy Transfer, Frequency Response, Inhomogeneity, Oscillations, Vertical Motion, Vibration Mode, Wentzel-Kramer-Brillouin Method

Scientific paper

The study concerns the oscillations and associated energy flux in a horizontally stratified medium permeated by a uniform vertical magnetic field parallel to a uniform gravitational field. Particular attention is given to the obvious applications to sunspots and the corona. In addition to the Alfven mode, the inhomogeneous analogs of the fast and slow MHD waves which propagate in a homogeneous medium are found. The boundary conditions and energy flux calculations that are appropriate for these modes are discussed, as are some general considerations of the series solutions themselves. The theory is then applied to the solar atmosphere. Numerical parameters typical of both sunspots and coronal hole regions are used in the investigations over a wide frequency range of the energy flux carried by such oscillations from the photosphere to the corona. It is concluded that the combined effects of stratification, partially transverse propagation, and the transition region make it unlikely that such modes dominate coronal energetics.

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