Computer Science
Scientific paper
Jan 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985nascp2358..183d&link_type=abstract
In its The Origin of Nonradiative Heating/Momentum in Hot Stars p 183-187 (SEE N85-17755 08-88)
Computer Science
Coronal Holes, Heating, Hot Stars, Magnetohydrodynamic Waves, Stellar Coronas, Stellar Models, Stellar Winds, Wave Propagation, Waveguides, Stellar Motions, Stellar Structure, Turbulence
Scientific paper
Magnetohydrodynamic (MHD) waves, driven by the large scale convective motions of the photosphere are suggested as a possible source of additional acceleration for the stellar wind. Most of the turbulent power in a coronal hole is carried by MHD waves with periods of a few hundred seconds or longer. This is evident from direct observations of turbulence in the solar photosphere, as well as in situ observations of turbulence in the solar wind. But waves with periods this long have wavelengths which are typically as large as the transverse scale of the coronal hole flux tube itself. For these waves boundary effects are important and the coronal hole must be treated as a waveguide. The propagation of MHD waves using this waveguide approach is discussed. The simple model presented demonstrates that coronal holes can act as waveguides for MHD waves. For typical solar parameters the waves are compressible and can generate a wave tensile force which tends to cancel at least part of the wave pressure force. This effect tends to decrease the efficiency of MHD wave acceleration.
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