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Magnetic field configuration in a flaring active region

Published online by Cambridge University Press:  24 July 2015

J. Palacios ,
L. A. Balmaceda  and
L. E. Vieira
J. Palacios
Affiliation:
Space Reseach Group–Space Weather, Departamento de Física y Matemáticas, Universidad de Alcalá, University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
L. A. Balmaceda
Affiliation:
Instituto Nacional de Pesquisas Espaciais (INPE), Avda. dos Astronautas, São José dos Campos–SP, 12227-010, Brazil Instituto de Ciencias Astronómicas, de la Tierra y el Espacio, ICATE-CONICET Avda. de España Sur 1512, J5402DSP, San Juan, Argentina
L. E. Vieira
Affiliation:
Instituto Nacional de Pesquisas Espaciais (INPE), Avda. dos Astronautas, São José dos Campos–SP, 12227-010, Brazil
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Abstract

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The Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) provides continuous monitoring of the Sun's vector magnetic field through full-disk photospheric data with both high cadence and high spatial resolution. Here we investigate the evolution of AR 11249 from March 6 to March 7, 2012. We make use of HMI Stokes imaging, SDO/SHARPs, the HMI magnetic field line-of-sight (LOS) maps and the transverse components of the magnetic field as well as LOS velocity maps in order to detect regions with significant flux emergence and/or cancellation. In addition, we apply the Local Correlation Tracking (LCT) technique to the total and signed magnetic flux data and derive maps of horizontal velocity. From this analysis, we were able to pinpoint localized shear regions (and a shear channel) where penumbrae and pore formation areas, with strong linear polarization signals, are stretched and squeezed, showing also important downflows and upflows. We have also utilized Hinode/SP data and compared them to the HMI-SHARPs and the HMI-Stokes spectrograms. The aforementioned shear channel seems to correspond well with the X-class flare main channel of March 7 2012, as observed in AIA/SDO 171, 304 and 1600 Å.

Keywords

Sun: photospheremagnetic fieldsflarestechniques: 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. 97 - 101
Copyright
Copyright © International Astronomical Union 2015 

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