HR: 0800h
AN: SH41A-1117    [Abstracts]
TI: Time-distance analysis of realistic simulations of solar convection
AU: * Georgobiani, D
EM: dali@pa.msu.edu
AU: Zhao, J
AF: Hansen Experimental Physics Laboratory, Stanford University, 455 via Palou, Stanford, CA 94305-4085 United States
AU: Benson, D
AF: Michigan State University, Physics and Astronomy Department, East Lansing, MI 48824 United States
AU: Stein, R F
AF: Michigan State University, Physics and Astronomy Department, East Lansing, MI 48824 United States
AU: Kosovichev, A G
AF: Hansen Experimental Physics Laboratory, Stanford University, 455 via Palou, Stanford, CA 94305-4085 United States
AU: Nordlund, A
AF: Niels Bohr Institute, Juliane Maries Vej 30, Copenhagen, DK-2100 Denmark
AB: The results of the new realistic large-scale simulations of solar turbulent convection provide an unprecedented opportunity to study solar oscillations and perform similar local helioseismology techniques as for the real solar data. The results offer an unique opportunity to compare the simulated flow fields with the flows and sounds speed variations inferred from the time-distance analysis. Applying some of the existing local helioseismology methods to the simulated solar convection and comparing to the observed results, one can validate the accuracy of these methods. We apply the time-distance analysis to the simulated data and successfully obtain the time-distance curve and travel time maps. Our travel times are consistent with the SOHO/MDI observations. The next step is to perform inversion to infer the interior flow fields at various depths and compare them with the simulated data in order to validate the model. This work is currently in progress.
DE: 7522 Helioseismology
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005