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Helioseismic Observations of Solar Convection Zone Dynamics

Published online by Cambridge University Press:  12 August 2011

Frank Hill ,
Rachel Howe ,
Rudi Komm ,
Irene González Hernández ,
Shukur Kholikov  and
John Leibacher
Frank Hill
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
Rachel Howe
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
Rudi Komm
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
Irene González Hernández
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
Shukur Kholikov
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
John Leibacher
Affiliation:
National Solar Observatory, Tucson, Arizona, USA85726
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Abstract

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The large-scale dynamics of the solar convection zone have been inferred using both global and local helioseismology applied to data from the Global Oscillation Network Group (GONG) and the Michelson Doppler Imager (MDI) on board SOHO. The global analysis has revealed temporal variations of the “torsional oscillation” zonal flow as a function of depth, which may be related to the properties of the solar cycle. The horizontal flow field as a function of heliographic position and depth can be derived from ring diagrams, and shows near-surface meridional flows that change over the activity cycle. Time-distance techniques can be used to infer the deep meridional flow, which is important for flux-transport dynamo models. Temporal variations of the vorticity can be used to investigate the production of flare activity. This paper summarizes the state of our knowledge in these areas.

Keywords

Sun: helioseismologySun: interiorSun: activity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 15 - 22
Copyright
Copyright © International Astronomical Union 2011

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