HR: 1330h
AN: SH42B-0537    [PDF]
TI: Solar Subsurface Synoptic Flow Maps by Time-Distance Helioseismology
AU: * Zhao, J
EM: junwei@quake.stanford.edu
AF: W. W. Hansen Experimental Physics Laboratory, Stanford University, 455 via Palou, Stanford, CA 94305 United States
AU: Kosovichev, A G
EM: sasha@quake.stanford.edu
AF: W. W. Hansen Experimental Physics Laboratory, Stanford University, 455 via Palou, Stanford, CA 94305 United States
AB: The synoptic flow maps have been made up to 12 Mm beneath the solar surface by use of time-distance helioseismology measurements and inversions. The study selects one Carrington rotation each year from 1996 to 2002, covering from solar minimum to maximum. The synoptic flow map has a high spatial resolution of 0.24 heliographic degree per pixel, and supergranular flows are able to be shown. Zonal and meridional flows, as well as the vorticity distribution are derived from such maps. It is found that after the subtraction of the solar minimum data, the residual meridional flows converge toward the activity belts, and migrate toward the equator together with the sunspot zones. Results are to be compared with those obtained from previous studies such as frequency splitting and ring-diagram analysis.
DE: 7522 Helioseismology
DE: 7524 Magnetic fields
DE: 7536 Solar activity cycle (2162)
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting