FREQUENCIES OF SOLAR OSCILLATIONS

We observed solar oscillations at different spatial scales using three different data sets acquired at Big Bear Solar Observatory during 1986-1987. Using these data, we present a new and more accurate table of the Sun's oscillation mode frequencies, v(nl), as a function of radial order n and spherical harmonic degree l. These frequencies are averages over azimuthal order m and therefore approximate the normal mode frequencies of a nonrotating, spherically symmetric Sun, near solar minimum. After including some results from other workers for completeness, the table presented here contains frequencies for most of the solar p- and f-modes with 0 less-than-or-equal-to l less-than-or-equal-to 1860, 0 less-than-or-equal-to n less-than-or-equal-to 26, and 1.0 less-than-or-equal-to v(nl) less-than-or-equal-to 5.3 mHz. Frequency uncertainties, sigma-nl, for individual multiplets are in some cases as low as 10 nHz, and the combined frequency uncertainty for the entire set is given by (SIGMA(nl)sigma(nl)-2)-1/2 approximately equals 700 pHz. Comparing the f-mode ridge with the theoretically expected frequencies, omega-2 = gk(h), we find that the observed frequencies are significantly less than expected for l > 1000, for which we have no explanation.