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Probing solar-cycle variations of magnetic fields in the convection zone using meridional flows

Published online by Cambridge University Press:  24 September 2020

Chia-Hsien Lin Open the ORCID record for Chia-Hsien Lin [Opens in a new window]  and
Dean-Yi Chou
Chia-Hsien Lin
Affiliation:
Graduate Institute of Space Science, National Central University, Taiwan email: chlin@jupiter.ss.ncu.edu.tw
Dean-Yi Chou
Affiliation:
Department of Physics, National Tsing-Hua University, Taiwan email: chou@phys.nthu.edu.tw
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Abstract

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Solar magnetic fields are believed to originate from the base of convection zone. However, it has been difficult to obtain convincing observational evidence of the magnetic fields in the deep convection zone. The goal of this study is to investigate whether solar meridional flows can be used to detect the magnetic-field effects. Meridional flows are axisymmetric flows on the meridional plane. Our result shows that the flow pattern in the entire convection zone changes significantly from solar minimum to maximum. The changes all centered around active latitudes, suggesting that the magnetic fields are responsible for the changes. The results indicate that the meridional flow can be used to detect the effects of magnetic field in the deep convection zone.

The results have been published in the Astrophysical Journal (lc2018).

Keywords

Sun: helioseismologySun: magnetic fieldsSun: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 160 - 165
Copyright
© International Astronomical Union 2020

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