A SEISMIC MODEL OF THE SUNS INTERIOR

We advance the method of frequency inversion revealing a more accurate seismic sounding of the solar core. We show that with the quoted obse rvational errors, it is possible to achieve a precision of approximate ly 10(-3) in the sound speed determination through most of the sun's i nterior. Only for r < 0.05 R. is the precision approximately 10(-2) Th e accuracy of the density and pressure determinations is only slightly worse. Such restrictions impose significant constraints on the micros copic physical data, i.e., opacities, nuclear-reaction cross sections, and diffusion coefficients, as well as on the solar age. The heliosei smic age is consistent with that from meteorites. The currently availa ble data for low-degree p-mode frequencies exhibit a scatter that is l arger than the quoted errors, and therefore the actual precision of se ismic inferences is less than what we report, especially for the solar core. We invert p-mode data to obtain a solar seismic model. Comparis on of the solar seismic model with current theoretical models shows a need for some refinements within the framework of the standard solar m odel. Only in the innermost part of the core (r < 0.05 R.) do we see a feature in the seismic sound speed that cannot easily be accounted fo r by refinements of the model. But the reality of the feature is by no means certain. We find no evidence supporting an astrophysical soluti on to the solar neutrino problem.