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Characteristics of Solar Proton Events Observed Near Earth and Stellar Activity Variations

Published online by Cambridge University Press:  27 November 2018

S. Aranya ,
T. E. Girish ,
G. Gopkumar  and
N. G. Nisha
S. Aranya
Affiliation:
Department of Physics, SN College, Sivagiri, Varkala 695145, India email: [email protected]
T. E. Girish
Affiliation:
Department of Physics, University College, Trivandrum 695034, India
G. Gopkumar
Affiliation:
Department of Physics, University College, Trivandrum 695034, India
N. G. Nisha
Affiliation:
Department of Physics, Government College for Women, Trivandrum 695014, India
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Abstract

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We could identify three categories of solar proton events (SPE) with distinct solar origin from an analysis of direct and indirect observations during the years 1561-2016 CE spanning 42 sunspot cycles. They are (i) 10 MeV SPE whose number of occurrences closely follow the sunspot cycles (ii) 30 MeV SPE which show secular changes with peaks near Gleissberg solar cycle minima and inferred to be associated with distinct enhancements in the efficiency of the solar dynamo and (iii) those associated with Impulsive and irregular solar activity changes such as the Carrington event of September 1859. The relevance of above results for stars exhibiting cyclic and irregular activity changes will be also discussed.

Keywords

Solar proton eventssunspot cyclessolar dynamoCarrington eventstellar activity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 265 - 266
Copyright
Copyright © International Astronomical Union 2018 

References

Davenport, J. R., Kipping, D. M., Sasselov, D., Matthews, J. M., & Cameron, C. 2016, ApJL, 829 (2), L31Google Scholar
Girish, T. E. & Gopkumar, G. 2010, arXiv preprint, arXiv.1011.4639 [phy-gen phys]Google Scholar
Olah, K., Kovari, Zs., Petrovay, K., Soon, W., Baliunas, S., Kollath, Z., & Vida, K., 2016, A&A, 590, A133Google Scholar
McCracken, K. G., Dreschoff, GAM, Zeller, E. J., Smart, D. F., & Shea, M. A., 2001a, JGR, 106, 21585–21598Google Scholar
McCracken, K. G., Dreschoff, GAM, Zeller, E. J., Smart, D. F., & Shea, M. A., 2001b, JGR, 106, 21599–21609Google Scholar
Smart, D. F., Shea, M. A., Dreschoff, G. A. M., McCracken, K. G., 2008, in Nellen, L. et al. (eds), Proc. 31st Int. Cosmic Ray Conf., Mexico, 1, 725–728Google Scholar