Three-dimensional simulations of solar oscillations: line profiles and asymmetries

Details Three-dimensional simulations of solar oscillations: line profiles and asymmetries Three-dimensional simulations of solar oscillations: line profiles and asymmetries

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.5605g&link_type=abstract

American Astronomical Society, 194th AAS Meeting, #56.05; Bulletin of the American Astronomical Society, Vol. 31, p.912

Physics

Scientific paper

In order to study spectral characteristics of the solar oscillations, we use the Stein-Nordlund 3d hydrodynamic code to generate lond temporal sequencies of realistically simulated upper layers of the solar convective zone. The simulation domain ranges from 0.5 Mm above the surface of tau =1 to 2.5 Mm below this surface, and is 6 Mm by 6 Mm wide. We have generated 24 hours of solar time. We calculate power spectra of the vertical velocity and temperature at different heights and the emergent intensity at the surface. Here, we present the profiles of velocity, intensity and temperature for both radial (l = 0) and first nonradial (l = 700) mode. We compare line profiles from the simulation with the power spectra of the Doppler velocity and continuum intensity from the SOHO/MDI observations. Both simulated and observed profiles demonstrate similar types of asymmetry, and the asymmetry reversal between the local quantities like velocity and temperature, and emergent intensity profiles is also present in the simulated data. The preliminary results are promising as they allow us to establish a connection between the observational data and realistic simulations, and enable us to understand better the physics of solar oscillations.

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