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Observational Signature of Tilt Quenching of Bipolar Magnetic Regions in the Sun

Published online by Cambridge University Press:  28 September 2023

Bibhuti Kumar Jha Open the ORCID record for Bibhuti Kumar Jha [Opens in a new window] ,
Bidya Binay Karak  and
Dipankar Banerjee Open the ORCID record for Dipankar Banerjee [Opens in a new window]
Bibhuti Kumar Jha
Affiliation:
Arybhatta Research Institute of Observational Sciences, Nainital-263001, India Email: [email protected]
Bidya Binay Karak
Affiliation:
Department of Physics, Indian Institute of Technology (BHU), Varanasi 221005, India
Dipankar Banerjee
Affiliation:
Arybhatta Research Institute of Observational Sciences, Nainital-263001, India Email: [email protected]
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Abstract

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It is believed that the tilt in the bipolar magnetic regions (BMRs) is produced due to a torque induced by the Coriolis force, acting on the diverging flow from the apex of the rising flux tube of the toroidal field in the solar convection zone (SCZ).The BMRs with a strong magnetic field are expected to have reduced tilt as they rise very quickly in the SCZ. This effect can provide the required nonlinear quenching mechanism to suppress the growth of magnetic filed in the dynamo models. Here, we use the magnetograms of the Michelson Doppler Imager (1996–2011) and Helioseismic and Magnetic Imager (2010–2018) to automatically detect the BMRs and look for the signature of tilt quenching. Based on the Bayesian inference method, our results show that the posterior distribution of quenching parameters is Gaussian, and the mean of this distribution agrees with the earlier findings.

Keywords

Sun: magnetic fields(Sun:) sunspotsSun: photospheremethods: statistical
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S372: The Era of Multi-Messenger Solar Physics , August 2022 , pp. 86 - 87
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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