Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-25T01:58:03.263Z Has data issue: false hasContentIssue false
  • English
  • Français

Exploring the Quenching of Bipolar Magnetic Region Tilts using AutoTAB

Published online by Cambridge University Press:  23 December 2024

Bibhuti Kumar Jha ,
Anu B. Sreedevi Open the ORCID record for Anu B. Sreedevi [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:
Southwest Research Institute, Boulder 80302, USA
Anu B. Sreedevi
Affiliation:
Department of Physics, Indian Institute of Technology (Banaras Hindu University), Varanasi 221005, India
Bidya Binay Karak
Affiliation:
Department of Physics, Indian Institute of Technology (Banaras Hindu University), Varanasi 221005, India
Dipankar Banerjee
Affiliation:
Aryabhatta Research Institute of Observational Sciences, Nainital 263002, Uttarakhand, India
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The tilt of the bipolar magnetic region (BMR) is crucial in the Babcock-Leighton process for the generation of the poloidal magnetic field in the Sun. We extend the work of Jha et al. (2020) and analyze the recently reported tracked BMR catalogue based on AutoTAB (Sreedevi et al. 2023) from Michelson Doppler Imager (1996–2011) and Helioseismic and Magnetic Imager (2010–2018). Using the tracked information of BMRs based on AutoTAB, we confirm that the distribution of Bmax reported by Jha et al. (2020) is not because of the BMRs are picked multiple times at the different phases of their evolution instead it is also present if we consider each BMRs only once. Moreover, we find that the slope of Joy’s law (〈γ0〉) initially increases slowly with the increase of Bmax. However, when Bmax >2.5 kG, γ0 decreases. The decrease of observed γ0 with Bmax provides a hint to a nonlinear tilt quenching in the Babcock-Leighton process.

Keywords

SunBipolar Magnetic RegionsSolar Dynamo
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 345 - 349
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Babcock, H. D. 1959, The Sun’s Polar Magnetic Field. ApJ, 130, 364.CrossRefGoogle Scholar
Babcock, H. W. 1961, The Topology of the Sun’s Magnetic Field and the 22-YEAR Cycle. ApJ, 133, 572.CrossRefGoogle Scholar
Biswas, A., Karak, B. B., & Cameron, R. 2022, Toroidal Flux Loss due to Flux Emergence Explains why Solar Cycles Rise Differently but Decay in a Similar Way. Phys. Rev. Lett., 129(24), 241102.CrossRefGoogle ScholarPubMed
Charbonneau, P. 2014, Solar dynamo theory. Ann. Rev. Astron. Astrophys., 52(1), 251–290.CrossRefGoogle Scholar
D’Silva, S. & Choudhuri, A. R. 1993, A theoretical model for tilts of bipolar magnetic regions. A&A, 272, 621.Google Scholar
Jha, B. K. 2022,. Long-term Study of the Sun and Its Implications to Solar Dynamo Models. PhD thesis, Pondicherry University.Google Scholar
Jha, B. K., Karak, B. B., & Banerjee, D. 2023, Observational Signature of Tilt Quenching of Bipolar Magnetic Regions in the Sun. IAU Symposium, 372, 86–87.Google Scholar
Jha, B. K., Karak, B. B., Mandal, S., & Banerjee, D. 2020, Magnetic Field Dependence of Bipolar Magnetic Region Tilts on the Sun: Indication of Tilt Quenching. ApJ Letters, 889(1), L19.CrossRefGoogle Scholar
Jha, B. K., Priyadarshi, A., Mandal, S., Chatterjee, S., & Banerjee, D. 2021, Measurements of Solar Differential Rotation Using the Century Long Kodaikanal Sunspot Data. Solar Phys., 296(1), 25.CrossRefGoogle Scholar
Karak, B. B., Jiang, J., Miesch, M. S., Charbonneau, P., & Choudhuri, A. R. 2014,a Flux Transport Dynamos: From Kinematics to Dynamics. Space Sci. Rev., 186a, 561–602.CrossRefGoogle Scholar
Karak, B. B. 2020, Dynamo Saturation through the Latitudinal Variation of Bipolar Magnetic Regions in the Sun. ApJ Letters, 901(2), L35.CrossRefGoogle Scholar
Karak, B. B. 2023, Models for the long-term variations of solar activity. Living Reviews in Solar Physics, 20(1), 3.CrossRefGoogle Scholar
Karak, B. B. & Miesch, M. 2017, Solar Cycle Variability Induced by Tilt Angle Scatter in a Babcock–Leighton Solar Dynamo Model. ApJ, 847, 69.CrossRefGoogle Scholar
Karak, B. B. & Miesch, M. 2018, Recovery from Maunder-like Grand Minima in a Babcock–Leighton Solar Dynamo Model. ApJ Letters, 860, L26.CrossRefGoogle Scholar
Lemerle, A., Charbonneau, P., & Carignan–Dugas, A. 2015, A Coupled 2 × 2D Babcock–Leighton Solar Dynamo Model. I. Surface Magnetic Flux Evolution. ApJ, 810, 78.CrossRefGoogle Scholar
Sreedevi, A., Jha, B. K., Karak, B. B., & Banerjee, D. 2023, AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions. ApJ Supplement, 268(2), 58.CrossRefGoogle Scholar
Sreedevi, A. B. & Jha, B. K. 2023, Automatic Algorithm for Tracking Bipolar Magnetic Regions. IAU Symposium, 372, 97–99.Google Scholar
Stenflo, J. O. & Kosovichev, A. G. 2012, Bipolar Magnetic Regions on the Sun: Global Analysis of the SOHO/MDI Data Set. ApJ, 745, 129.CrossRefGoogle Scholar