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Towards physics-based helioseismic inversions of subsurface sunspot structure

Published online by Cambridge University Press:  26 August 2011

D. C. Braun ,
A. C. Birch ,
A. D. Crouch  and
M. Rempel
D. C. Braun
Affiliation:
NorthWest Research Assoc, CoRA Div, 3380 Mitchell Ln, Boulder, CO, USA email: dbraun@cora.nwra.com, aaronb@cora.nwra.com, ash@cora.nwra.com
A. C. Birch
Affiliation:
NorthWest Research Assoc, CoRA Div, 3380 Mitchell Ln, Boulder, CO, USA email: dbraun@cora.nwra.com, aaronb@cora.nwra.com, ash@cora.nwra.com
A. D. Crouch
Affiliation:
NorthWest Research Assoc, CoRA Div, 3380 Mitchell Ln, Boulder, CO, USA email: dbraun@cora.nwra.com, aaronb@cora.nwra.com, ash@cora.nwra.com
M. Rempel
Affiliation:
NCAR, HAO Div, 3080 Center Green Dr, Boulder, CO, USA email: rempel@ucar.edu
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Abstract

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Numerical computations of wave propagation through sunspot-like magnetic field structures are critical to developing and testing methods to deduce the subsurface structure of sunspots and active regions. We show that helioseismic analysis applied to the MHD sunspot simulations of Rempel and collaborators, as well as to translation-invariant models of umbral-like fields, yield wave travel-time measurements in qualitative agreement with those obtained in real sunspots. However, standard inversion methods applied to these data fail to reproduce the true wave-speed structure beneath the surface of the model. Inversion methods which incorporate direct effects of the magnetic field, including mode conversion, may be required.

Keywords

Sun: helioseismologySun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 379 - 383
Copyright
Copyright © International Astronomical Union 2011

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