Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..49e&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Computer Science
Scientific paper
We presented results of analysis of p-modes travel time variation via solar activity cycle using Multiple Bounce Travel Time Analysis (MBTTA) method. It is shown that travel time of different wave packets exhibits pattern which correlates with solar magnetic activity. We extended MBTTA method by including analysis of frequencies of different wave packets. The difference of travel time variation averaged over high and low phase velocity was analysed to search for small variation caused by perturbation in solar interior. The results show small amplitude variation of this difference with solar cycle and might be interpreted as a manifestation of solar cycle variation originated near the base of the convection zone (BCZ). Comparison with modelling suggests that if this variation caused by change of magnetic fields at the BCZ then the magnitude of this change imply the strength of magnetic fields as high as 3.0-3.5×10^5 Gauss.
Egamberdiev Sh. A.
Serebryanskiy A. V.
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