Physics
Scientific paper
Dec 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..265k&link_type=abstract
In ESA, Seismology of the Sun and Sun-Like Stars p 265-268 (SEE N89-25819 19-92)
Physics
2
Damping, Magnetic Flux, P Waves, Solar Flux Density, Solar Magnetic Field, Eddington Approximation, Stellar Models, Sunspots, Wave Propagation
Scientific paper
In a generalization of a work by Mihalas and Mihalas (1983) describing the propagation of compressive disturbances in a radiating fluid, the dynamical influence of a uniform magnetic field is included. The radiating fluid is treated to be gray, in LTE and assumed to obey the Eddington approximation. Results are applied to the interaction of solar p-modes with sunspots in the context of a simple model developed by Abdelatif and Thomas (1987). For physical conditions representative of the solar envelope and for a variety of embedded magnetic structures, the temperature fluctuations associated with compressive waves are reduced inside the magnetic regions. Hence, radiative damping of these disturbances is suppressed to an extent that depends upon the nature of the mode (fast or slow magnetoacoustic) and the propagation direction relative to the uniform background field. This conclusion raises interesting predictions concerning the observational signatures of compressive waves in the solar envelope.
Bogdan Thomas. J.
Knoelker Michael
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