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Comparison of subsurface sound-speed structures of three active regions

Published online by Cambridge University Press:  01 November 2006

S. Couvidat ,
A. C. Birch ,
S. P. Rajaguru  and
A. G. Kosovichev
S. Couvidat
Affiliation:
HEPL, Stanford University and CoRA, NWRA, Boulder email: couvidat@stanford.edu
A. C. Birch
Affiliation:
HEPL, Stanford University and CoRA, NWRA, Boulder email: couvidat@stanford.edu
S. P. Rajaguru
Affiliation:
HEPL, Stanford University and CoRA, NWRA, Boulder email: couvidat@stanford.edu
A. G. Kosovichev
Affiliation:
HEPL, Stanford University and CoRA, NWRA, Boulder email: couvidat@stanford.edu
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Abstract

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We analyze three solar active regions observed with the MDI instrument onboard SoHO (Scherrer et al. 1995). We apply the time-distance helioseismology formalism to derive the travel times of acoustic waves propagating through these active regions. The inversion of these acoustic travel times gives us access to the 3D sound-speed structure below the sunspots. We compare the main characteristics of these inversion results as a function of the active region size and magnetic field strength.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 75 - 76
Copyright
© 2006 International Astronomical Union