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Solar cycle and quasi-biennial variations in helioseismic frequencies

Published online by Cambridge University Press:  18 July 2013

Sushanta C. Tripathy ,
Kiran Jain ,
Rosaria Simoniello ,
Frank Hill  and
Sylvaine Turck-Chièze
Sushanta C. Tripathy
Affiliation:
National Solar Observatory, Tucson, AZ 85719, USA email: stripathy@nso.edu, kjain@nso.edu, fhill@nso.edu
Kiran Jain
Affiliation:
National Solar Observatory, Tucson, AZ 85719, USA email: stripathy@nso.edu, kjain@nso.edu, fhill@nso.edu
Rosaria Simoniello
Affiliation:
Laboratoire AIM, CEA/DSM-CNRS-I|universite Paris Diderot; CEA, IRFU, SAp, center de Saclay, F-91191, Gif-sur-Yvette, France email: rosaria.simoniello@cea.fr, sylvaine.turck-chieze@cea.fr
Frank Hill
Affiliation:
National Solar Observatory, Tucson, AZ 85719, USA email: stripathy@nso.edu, kjain@nso.edu, fhill@nso.edu
Sylvaine Turck-Chièze
Affiliation:
Laboratoire AIM, CEA/DSM-CNRS-I|universite Paris Diderot; CEA, IRFU, SAp, center de Saclay, F-91191, Gif-sur-Yvette, France email: rosaria.simoniello@cea.fr, sylvaine.turck-chieze@cea.fr
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Abstract

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The prolonged period of solar minimum between cycles 23 and 24 has invoked a great deal of interest to understand the origin of the unusually low solar activity. Even though the origin of solar activity is believed to lie in the shear layer at the base of the convection zone, the analysis of helioseismic data seem to orientate us toward the near surface. In this context, we analyze the signature of the quasi-biennial periodicity seen in the oscillation frequencies which may provide additional constraints on the solar dynamo models.

Keywords

Sun: helioseismology – Sun: interior – Sun: oscillations

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