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Full Stokes observations in the He i 1083 nm spectral region covering an M3.2 flare

Published online by Cambridge University Press:  24 July 2015

Christoph Kuckein ,
Manuel Collados ,
Rafael Manso Sainz  and
Andrés Asensio Ramos
Christoph Kuckein
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), D-14482 Potsdam, Germany email: ckuckein@aip.de
Manuel Collados
Affiliation:
Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
Rafael Manso Sainz
Affiliation:
Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
Andrés Asensio Ramos
Affiliation:
Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
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Abstract

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We present an exceptional data set acquired with the Vacuum Tower Telescope (Tenerife, Spain) covering the pre-flare, flare, and post-flare stages of an M3.2 flare. The full Stokes spectropolarimetric observations were recorded with the Tenerife Infrared Polarimeter in the He i 1083.0 nm spectral region. The object under study was active region NOAA 11748 on 2013 May 17. During the flare the chomospheric He i 1083.0 nm intensity goes strongly into emission. However, the nearby photospheric Si i 1082.7 nm spectral line profile only gets shallower and stays in absorption. Linear polarization (Stokes Q and U) is detected in all lines of the He i triplet during the flare. Moreover, the circular polarization (Stokes V) is dominant during the flare, being the blue component of the He i triplet much stronger than the red component, and both are stronger than the Si i Stokes V profile. The Si i inversions reveal enormous changes of the photospheric magnetic field during the flare. Before the flare magnetic field concentrations of up to ~1500 G are inferred. During the flare the magnetic field strength globally decreases and in some cases it is even absent. After the flare the magnetic field recovers its strength and initial configuration.

Keywords

Sun: flaresSun: photosphereSun: chromosphereSun: magnetic fieldstechniques: polarimetric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Symposium S305: Polarimetry: From the Sun to Stars and Stellar Environments , December 2014 , pp. 73 - 78
Copyright
Copyright © International Astronomical Union 2015 

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