Abstract
By analyzing the observed frequencies of solar P-mode pressure waves, it has been possible to obtain detailed knowledge about the density, rate of rotation, temperature, pressure and composition of the sun in its interior. The frequencies of these oscillations is obtained by observing the Doppler shifting of the Fraunhofer absorption lines in the sun's optical spectrum. The sun is modeled as a self-gravitating ideal gas. The effects of convection, rotation and magnetic-field interacttons math the plasma are neglected. The observed cies of oscillation lie 'in the range of approximately 16OO-4800 []Hz.. P-waves oscillating in this frequency range allows for irnvng of the sun's s c down to the core. 'Me intermediate P-modes with I-values between 20 and 100 are used to image the sun's s in the outer 30 percent of its radius. This corresponds to the approxffnate depth of the lower boundary of the sun's convection zone.
Brown, Terry T (1996). A comparative study of imtermediate P-mode pressure-wave propagation in the sun. Master's thesis, Texas A&M University. Available electronically from
https : / /hdl .handle .net /1969 .1 /ETD -TAMU -1996 -THESIS -B757.