Realistic 3D numerical simulations of solar convection are capable of reproducing the excitation of solar oscillations by turbulent convection. Continuing our investigations, we calculate velocity power spectra for high angular degree modes that have their lower turning points within the shallow simulation domain. We find excellent agreement between the observed SOHO/MDI and simulated power spectra in frequency, amplitude and mode width. However, surprisingly at lower frequencies, the noise level in the model is much higher than in the Sun.
|Original language||English (US)|
|Number of pages||4|
|Journal||European Space Agency, (Special Publication) ESA SP|
|State||Published - Dec 1 2004|
All Science Journal Classification (ASJC) codes
- Aerospace Engineering