Models of the solar oscillations
Abstract
The shallow upper layer of the solar convection zone is simulated using the three-dimensional hydrodynamic code of Stein & Nordlund. The simulation oscillation modes behave similarly to the SOHO/MDI observations; namely, they have the same asymmetries and phase relations. Therefore, one can study the properties of the modes from the simulations to investigate behavior below the surface, which cannot be observed directly. The asymmetry of the line profiles varies with depth. At the surface, the velocity asymmetry is the same as in the SOHO/MDI observations, but deeper down it becomes flipped in comparison to the surface asymmetry. This behavior is well represented by the simple model of a potential well with the source inside (or outside). The simulations can be used to determine the depth of the driving at different frequencies, while the simulation modes show a strong correlation of excitation with emergent intensity.
- Publication:
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SOHO 10/GONG 2000 Workshop: Helio- and Asteroseismology at the Dawn of the Millennium
- Pub Date:
- January 2001
- Bibcode:
- 2001ESASP.464..583G
- Keywords:
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- NUMERICAL SIMULATIONS;
- SOLAR CONVECTION;
- SOLAR OSCILLATIONS