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Diagnostics of non-thermal-distributions from solar flare EUV line spectra

Published online by Cambridge University Press:  24 September 2020

Elena Dzifčáková Open the ORCID record for Elena Dzifčáková [Opens in a new window] ,
Alena Zemanová ,
Jaroslav Dudík  and
Juraj Lörinčík
Elena Dzifčáková
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
Alena Zemanová
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
Jaroslav Dudík
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
Juraj Lörinčík
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
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Abstract

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Spectral line intensities observed by the Extreme Ultraviolet Variability Experiment (EVE) on board the Solar Dynamics Observatory (SDO) during 2012 March 9 M6.3 flare were used to diagnose a presence of a non-thermal electron distribution represented by a κ-distribution. The diagnosed electron densities ($\approx 2 \times {10^{11}}{\rm{c}}{{\rm{m}}^{ - 3}}$) are affected only a little by the presence of the non-thermal distribution, and are within the uncertainties of observation. On the other hand, the temperature diagnostics based on the line ratios involving different ionization degrees is strongly affected by the type of the electron distribution. The distribution functions diagnosed from relative Fe line intensities demonstrate the presence of strongly non-thermal distributions during the impulsive phase of the flare and later their gradual thermalization.

Keywords

Sun: flaresSun: UV radiationtechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 414 - 417
Copyright
© International Astronomical Union 2020

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