Physics
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..135..131b&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 135, Sept. 1991, p. 131-161.
Physics
35
Interstellar Magnetic Fields, Magnetohydrodynamic Waves, Stellar Atmospheres, Stellar Winds, Asymptotic Methods, Mathematical Models, Wave Propagation, Wave Reflection, Wentzel-Kramer-Brillouin Method
Scientific paper
The present study examines a mathematical model for undamped toroidal small-amplitude Alfven waves in a spherically-symmetric or equatorial stellar wind. The behavior of the solutions at large distances is explained in terms of the amplitude ratio, which is linked to the integral reflection effect. Consideration is given to the validity of the WKB approximation in different regions of the flow. It is shown that, for a wide range of frequencies, it is incorrect to assume no inward propagating waves or to use the WKB approximation at large distances to the star. Some numerical results are presented using a cool-wind model. It is argued that they express qualitatively the features of the Alfven waves in any stellar wind. The numerical solutions show that, up to distances about 200-300 stellar radii, the wave coupling does not change the outward propagating wave amplitude very much, keeping it less than 50 percent larger than its WKB approximate estimate.
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