Mechanical wave-energy flux in magnetoatmospheres: Discrete and continuous spectra - Mechanical wave energy flux in magnetoatmospheres

Details Mechanical wave-energy flux in magnetoatmospheres: Discrete and continuous spectra - Mechanical wave energy flux in magnetoatmospheres Mechanical wave-energy flux in magnetoatmospheres: Discrete and continuous spectra - Mechanical wave energy flux in magnetoatmospheres

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..78..293a&link_type=abstract

Astrophysics and Space Science, vol. 78, no. 2, Aug. 1981, p. 293-350.

Astronomy and Astrophysics

Astrophysics

11

Astrophysics, Atmospheric Heat Budget, Continuous Spectra, Energy Distribution, Line Spectra, Solar Atmosphere, Stellar Atmospheres, Atmospheric Models, Atmospheric Stratification, Group Velocity, Magnetic Fields

Scientific paper

Media for which the restoring forces of buoyancy, compressibility, and magnetic tension/pressure are important in sustaining wave motion are discussed. After discussing the equilibrium and stability of such systems and certain mathematical properties of a particular system, theory is developed which enables expressions to be written down for the mechanical wave energy flux associated with wave motion arising from a transient source. These analytic expressions are extremely general and contain contributions from the continuous and discrete frequency spectra, corresponding respectively to freely propagating and trapped (or surface) waves. These fluxes are evaluated for diverse ranges of magnetic field, horizontal wave number, characteristic source times and frequency, for a simple constant-parameter atmosphere. The source is taken to be a transient fluctuation of the lower boundary, which in turn is taken to be located at the level tau5000 = 0.08 in the solar atmosphere. The relative distribution of wave energy flux in the various modes is analyzed in the context of solar physics parameters. The possible significance of 'leaky' modes arising from supergranular or other flow for the local flux balance in the solar chromosphere is discussed.

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