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Super Flares in M Stars and Associated Characteristics of Active Regions and Magnetic Fields

Published online by Cambridge University Press:  23 December 2024

M. Kumar Varnana Open the ORCID record for M. Kumar Varnana [Opens in a new window] ,
T. E. Girish ,
Thara N. Sathyan ,
V. G. Haritha  and
G. Gopkumar
M. Kumar Varnana*
Affiliation:
Department of Physics, Mar Ivanios College, Trivandrum, Kerala-695015
T. E. Girish*
Affiliation:
Department of Physics, University College, Trivandrum, Kerala-695034
Thara N. Sathyan*
Affiliation:
Department of Physics, University College of Engineering Kariavattom, Trivandrum, Kerala-695581
V. G. Haritha*
Affiliation:
Department of Physics, College of Engineering, Trivandrum, Kerala-695016
G. Gopkumar*
Affiliation:
Department of Physics, University College, Trivandrum, Kerala-695034
*
email: [email protected]
emails: [email protected]; [email protected]
email: [email protected]
email: [email protected]
emails: [email protected]; [email protected]
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Abstract

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Observations of super flare occurrence (with energy 1033–1036 erg)s in low mass stars like M dwarfs still remains as a puzzle. In this paper we have inferred the typical sizes and characteristics of magnetic fields associated with active regions in M dwarfs responsible for these super flares. This is done by extrapolation of physical conditions associated with largest solar flares. The average poloidal and toroidal magnetic fields near the surface of selected M dwarfs will be also inferred in this context.

Keywords

Super flaresM dwarfsSolar flaresActive regionsMagnetic fields
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. 375 - 378
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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