Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..583g&link_type=abstract
In: Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and asteroseismology at the dawn of the millennium, 2-6 October 2000,
Computer Science
1
Numerical Simulations, Solar Convection, Solar Oscillations
Scientific paper
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.
Georgobiani Dali
Nordlund Aake
Stein Robert F.
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