The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models

Details The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993cha%26a..17...74c&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 17, Issue 1, p. 74-83.

Astronomy and Astrophysics

Astrophysics

Solar Oscillation, Solar Structure

Scientific paper

In this paper, the adiabatic p-mode eigenfrequencies for five solar convective envelope models are calculated, using Xiong's nonlocal convection theory. At the precision level of one percent, they are well consistent with observation. From the plotting of Δν(= νobs -νcal) vs. ν, it is obvious for the models with smaller convection parameter c1 (the models I and II), that the frequency differences fall into two distinct groups. For the modes with l > 60, the differencies decrease as the frequency increases, distributing in an inclined narrow strip. This indicates that the main error source is located in the out- ermost 5% Rsolar region of the models, possibly due to the nonadiabatic effects and the uncertainty in the equation of state. For the modes with l <= 60, the theoretical eigenfrequencies are systematically smaller than the observed ones, implying that another error source locates at the bottom of the solar convection zone and the overshooting region below. It may be most likely interpreted by the existence of a magnetic field of 103- 104 gauss in the lower part of the solar convection zone.

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