Computer Science – Sound
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0704p&link_type=abstract
American Astronomical Society, SPD meeting #40, #7.04; Bulletin of the American Astronomical Society, Vol. 41, p.813
Computer Science
Sound
Scientific paper
Investigation of the interaction of MHD waves with sunspots is very important for correct interpretation of local helioseismology data and sunspot seismology. We compare results of 3D numerical simulations of propagation of the MHD waves in subphotospheric and photospheric layers of sunspots. Two self-consistent magnetohydrostatic background models of sunspots based on a solution of Pizzo and a self-similar solution of Low were chosen as the background models. We consider the models with different magnetic field and sound-speed depth structures, extended into the deep interior and shallow. The MHD waves form two distinct classes: magnetoacoustic and magnetogravity modes. There are similarities and differences in wave behavior in the sunspot models. It is shown, that inside the sunspot magnetoacoustic and magnetogravity waves are not spatially separated unlike the case of the horizontally uniform magnetic field. The sunspot causes anisotropy of the amplitude distribution along the wavefront and changes the shape of the wavefront. The amplitude of the waves is reduced inside the sunspot. This effect is stronger for the magnetogravity waves than for the magnetoacoustic waves. The shape of the wavefront of the magnetogravity waves is distorted stronger as well. For the deep sunspot model the anisotropy is stronger for both magnetoacoustic and magnetogravity waves than for the shallow model. These effects cause changes in wave travel times. A strong Alfven wave is generated at the wave source location in the deep sunspot model. This wave is almost unnoticeable in the shallow model.
Kosovichev Aleksandr G.
Parchevsky Konstantin
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