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Initiation and chromospheric effects of a M1.0 class solar flare from high-resolution multi-wavelength observations

Published online by Cambridge University Press:  12 September 2017

V. M. Sadykov ,
A. G. Kosovichev ,
I. N. Sharykin ,
I. V. Zimovets  and
S. Vargas Dominguez
V. M. Sadykov
Affiliation:
Department of Physics, New Jersey Institute of Technology, Newark, NJ 07102, USA email: vsadykov@njit.edu
A. G. Kosovichev
Affiliation:
Department of Physics, New Jersey Institute of Technology, Newark, NJ 07102, USA email: vsadykov@njit.edu NASA Ames Research Center, Moffett Field, CA 94035, USA W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
I. N. Sharykin
Affiliation:
Space Research Institute (IKI) of Russian Academy of Sciences, Moscow 117997, Russia
I. V. Zimovets
Affiliation:
Space Research Institute (IKI) of Russian Academy of Sciences, Moscow 117997, Russia
S. Vargas Dominguez
Affiliation:
Universidad Nacional de Colombia, Sede Bogotá, Observatorio Astronómico, Carrera 45 # 26-85, Bogotá, Colombia
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Abstract

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Initiation and development of a M 1.0 class flare of June 12, 2014, was observed by space and ground-based telescopes, including EUV and X-ray imaging spectroscopy by IRIS and RHESSI, and high-resolution optical imaging by 1.6 m New Solar Telescope (NST). Analyzing the NST data, we found small-scale loop-like structures in the region of the magnetic field Polarity Inversion Line (PIL), the emergence and interaction of which caused photospheric brightenings temporarily coinciding with hard X-ray impulses. Detailed studies of the PIL region reveal signatures of photospheric plasma downflows and dissipation of electric currents. The reconstructed magnetic field topology shows a bundle of lines connecting the PIL region with the flare ribbons which were places of chromospheric evaporation observed by IRIS. The observations suggest a scenario with the primary energy release processes located in the low atmospheric layers of the PIL, energizing the overlying large-scale magnetic structure and causing “gentle” chromospheric evaporation.

Keywords

Sun: flaresSun: magnetic fieldsSun:photosphereSun: chromosphereSun: transition region
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 103 - 108
Copyright
Copyright © International Astronomical Union 2017 

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