The solar p-mode frequencies represent a unique source of observational information about the physical properties of the solar interior, including the equation of state (EPS). The influence of possible uncertainties in the EOS on the frequencies is small, and mixed with a variety of possible uncertainties in solar structure and physics of the oscillations. This paper describes a technique aimed at separating the effects of the EOS in the information contained in the intermediate-degree data by extracting some functions, or ‘tracers’, sensitive to the EOS, and insensitive, as far as possible, to the irrelevant effects. The possibilities of the technology are examined by testing a variety of solar envelope models computed with four versions of EOS, in increasing degree of sophistication: (1) EOS of partially ionized ideal gas; (2) EOS with Debye–Hüeckel electrostatic corrections; (3) EOS with short-range corrections to the Debye–Hüeckel term, and (4) the most recent (Mihalas, Hummer & Däppen) MHD equation of state. By comparing the models with observational data, we (i) discuss the effects of the electrostatic corrections, and (ii) draw first tentative conclusions on two more elaborate versions of the EOS.
No takes yet. Share an insight, caveat, or question.
Воронцов et al. (1992) studied this question.