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On origin of active/inactive branches on moderate rotating solar analogs

Published online by Cambridge University Press:  23 December 2024

Valery V. Pipin Open the ORCID record for Valery V. Pipin [Opens in a new window]
Valery V. Pipin*
Affiliation:
Institutte solar-terrestrial physics, Irkutsk, 6604033, Russia
*
email: [email protected]
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Abstract

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The fast rotating solar analogs show a decrease of the dynamo period with an increase of the rotation rate for the moderate stellar rotation periods in the range between 10 and 25 days. Simultaneously, observations indicate two branches: the “in-active” branch stars shows short dynamo cycles and the active branch stars show the relatively long magnetic cycles. We suggest that this phenomenon can be produced by effect of the doubling frequency of the dynamo waves, which is due to excitation of the second harmonic. It is generated because of the nonlinear B2 effects in the large-scale dynamo.

Keywords

stellar dynamomagnetic activity cycles
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. 174 - 178
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Brandenburg, A., Mathur, S., & Metcalfe, T. S. 2017, Evolution of co-existing long and short period stellar activity cycles. ApJ, 845(1), 79.CrossRefGoogle Scholar
Lehtinen, J., Jetsu, L., Hackman, T., Kajatkari, P., & Henry, G. W. 2016, Activity trends in young solar-type stars. A&A, 588, A38.Google Scholar
Noyes, R. W., Weiss, N. O., & Vaughan, A. H. 1984, The relation between stellar rotation rate and activity cycle periods. ApJ, 287, 769–773.CrossRefGoogle Scholar
Parker, E. N. 1979,. Cosmical magnetic fields: Their origin and their activity. Oxford: Clarendon Press.Google Scholar
Pipin, V. V. 2021, Solar dynamo cycle variations with a rotational period. MNRAS, 502(2), 2565–2581.CrossRefGoogle Scholar
Pipin, V. V. 2023, Spatio-temporal non-localities in a solar-like mean-field dynamo. MNRAS, 522(2), 2919–2927.CrossRefGoogle Scholar
Rheinhardt, M. & Brandenburg, A. 2012, Modeling spatio-temporal nonlocality in mean-field dynamos. Astronomische Nachrichten, 333, 71–77.CrossRefGoogle Scholar
Soon, W. H., Baliunas, S. L., & Zhang, Q. 1994, Variations in surface activity of the sun and solar-type stars. Solar Phys., 154, 385–391.CrossRefGoogle Scholar
Stix, M. Dynamo Theory and the Solar Cycle. In Bumba, V. & Kleczek, J., editors, Basic Mechanisms of Solar Activity 1976, volume 71, 367.CrossRefGoogle Scholar
Warnecke, J. 2018, Dynamo cycles in global convection simulations of solar-like stars. A&A, 616, A72.Google Scholar
Yoshimura, H. 1975, Solar-cycle dynamo wave propagation. ApJ, 201, 740–748.CrossRefGoogle Scholar