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Spectroscopic UV observations of M1.0 class solar flare from IRIS satellite

Published online by Cambridge University Press:  09 September 2016

Viacheslav M Sadykov ,
Alexander G Kosovichev ,
Ivan N Sharykin  and
Santiago Vargas Dominguez
Viacheslav M Sadykov
Affiliation:
New Jersey Institute of Technology, Newark, NJ 07102, USA email: vsadykov@njit.edu
Alexander G Kosovichev
Affiliation:
New Jersey Institute of Technology, Newark, NJ 07102, USA email: vsadykov@njit.edu NASA Ames Research Center, Moffet Field, CA 94035, USA
Ivan N Sharykin
Affiliation:
Space Research Institute (IKI), Moscow 117997, Russia
Santiago Vargas Dominguez
Affiliation:
Observ. Astron. Univ. Nacional de Colombia, Bogotá 111321, Colombia
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Abstract

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This work presents an analysis of UV spectroscopic observations from the IRIS satellite of an M1.0 class flare occurred on 12 June 2014 in active region NOAA 12087. Our analysis of the IRIS spectra and Slit-Jaw images revealed presence of a strongly redshifted chromospheric jet before the flare. We also found strong emission of the chromospheric lines, and studied the C II 1334.5 Å line emission distribution in details. A blueshift of the Fe XXI line across the flaring region corresponds to evaporation flows of the hot chromospheric plasma with a speed of 50 km/s. Although the enhancement of the C II line integrated redshift correlates with the flare X-ray emission, we classify the evaporation as of a “gentle” type because of its long time scale and subsonic velocities. Analysis of X-ray data from the RHESSI satellite showed that both, an injection of accelerated particles and a heat flux from the energy release site can explain the energetics of the observed event.

Keywords

Sun: activityflaresmagnetic fieldsatmosphereUV radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 64 - 67
Copyright
Copyright © International Astronomical Union 2016 

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