The interfacial F mode in a spherical solar model
Abstract
The solar f modes are a branch of oscillations characterized by a close correspondence between their measured dispersion relation and that predicted for a pure surface gravity wave: omega^2=gk where g is the surface gravity of the Sun. However, there is now substantial evidence for deviations from this simple behaviour. We consider the hypothesis of Rosenthal & Gough that the f modes are characterized better as an interfacial wave propagating at the chromosphere-corona transition. Using a standard solar interior model, a semi-empirical atmospheric model, and a parametrized transition region model as our equilibrium state, we solve the linearized oscillation equations for the interfacial f mode. We find that the frequencies of the interfacial f mode differ from those of the classical f mode only at very high degrees. We conclude that the interfacial f-mode theory may be the correct explanation for the very high-degree data, but that some other mechanism is required to explain the lower degree data.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- October 1995
- DOI:
- 10.1093/mnras/276.3.1003
- Bibcode:
- 1995MNRAS.276.1003R
- Keywords:
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- SUN: ATMOSPHERE;
- SUN: OSCILLATIONS