Barry J. Labonte

TL;DR: In this article, a series of observations designed to probe the nature of sunspots by detecting their influence on high-degree p-mode oscillations in the surrounding photosphere is presented.

TL;DR: In this article, the effect of local regions on solar p-mode oscillations was measured and measured in and around several sunspots, and it was found that active regions absorb an energy flux of the order of about 10 to 7th ergs/sq cm s, which is about 0.0001 of the sunspot energy deficit.

TL;DR: The Mees Solar Observatory on Haleakala, Maui as discussed by the authors uses a 28 cm aperture telescope, a polarization modulator, a tunable Fabry-Perot filter, CCD cameras and control electronics.

TL;DR: In this paper, the acoustic scattering properties of a large sunspot are determined from a Fourier-Hankel decomposition of p-mode amplitudes as measured from a 68hr subset of a larger set of observations made at the South Pole in 1988.

Abstract: It is shown that the use of a two-parameter limbshift and a meridional flow velocity fits solar velocity data better than the standard analysis defined by Howard et al. (1980). The data used are the coarse residual velocity arrays, with 34 equal intervals in both sine latitude and sine longitude. There are a total of 2899 full-disk observations between January 1, 1967, and December 12, 1980. The original velocity fields are reconstructed by adding into the residual arrays the large-scale patterns that were measured and removed on a daily basis by a standard reduction. Tests of this reconstituded data set show that no significant errors are introduced in the analysis of large-scale velocity fields. The results of the analysis presented here imply that the study of solar velocity pattern at the level of a few m/s requires that magnetic regions be treated separately from nonmagnetic regions.