Hostname: page-component-5c6d5d7d68-thh2z Total loading time: 0 Render date: 2024-09-02T05:23:47.254Z Has data issue: false hasContentIssue false
  • English
  • Français

Topological study of active region 11158

Published online by Cambridge University Press:  06 January 2014

Jie Zhao ,
Hui Li ,
Etienne Pariat ,
Brigitte Schmieder ,
Yang Guo  and
Thomas Wiegelmann
Jie Zhao
Affiliation:
Purple Mountain Observatory, CAS, 2 West Beijing Road, Nanjing 210008, China email: nj.lihui@pmo.ac.cn Key Laboratory of Dark Matter and Space Astronomy, CAS, Nanjing 210008, China
Hui Li
Affiliation:
Purple Mountain Observatory, CAS, 2 West Beijing Road, Nanjing 210008, China email: nj.lihui@pmo.ac.cn Key Laboratory of Dark Matter and Space Astronomy, CAS, Nanjing 210008, China
Etienne Pariat
Affiliation:
LESIA, Observatoire de Paris, Section de Meudon, F-92195, Meudon Principal Cedex, France
Brigitte Schmieder
Affiliation:
LESIA, Observatoire de Paris, Section de Meudon, F-92195, Meudon Principal Cedex, France
Yang Guo
Affiliation:
School of Astronomy & Space Science, Nanjing University, Nanjing 210093, China
Thomas Wiegelmann
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

With the cylindrical equal area (CEA) projection data from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO), we reconstructed the three-dimensional (3D) magnetic fields in the corona, using a non-linear force-free field (NLFFF) extrapolation method every 12 minutes during five days, to calculate the squashing degree factor Q in the volume. The results show that this AR has an hyperbolic flux tube (HFT) configuration, a typical topology of quadrupole, which is stable even during the two large flares (M6.6 and X2.2 class flares).

Keywords

coronaflaresmagnetic topology
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 479 - 480
Copyright
Copyright © International Astronomical Union 2013 

References

Aulanier, G., Pariat, E., & Démoulin, P. 2005, A&A, 444, 961Google Scholar
Berger, M. A. 1991, Advances in Solar System Magnetohydrodynamics, 241Google Scholar
Pariat, E. & Démoulin, P. 2012, A&A, 541, A78Google Scholar
Titov, V. S., Hornig, G., & Démoulin, P. 2002, JGR, 107, 1164CrossRefGoogle Scholar
Titov, V. S., Galsgaard, K., & Neukirch, T. 2003, ApJ, 582, 1172CrossRefGoogle Scholar