Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-11-28T13:51:15.550Z Has data issue: false hasContentIssue false

Hinode magnetic-field observations of solar flares for exploring the energy storage and trigger mechanisms

Published online by Cambridge University Press:  09 September 2016

Toshifumi Shimizu
Affiliation:
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan email: [email protected] Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033Japan email: [email protected]
Satoshi Inoue
Affiliation:
Max-Planck Institute for Solar System Research, BT2.E4.120, Justus-von-Liebig-Weg 3 37077, Göttingen, Germany email: [email protected]
Yusuke Kawabata
Affiliation:
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan email: [email protected] Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033Japan email: [email protected]
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.

The spectro-polarimeter in the Hinode Solar Optical Telescope (SOT) is one of the powerful instruments for the most accurate measurements of vector magnetic fields on the solar surface. The magnetic field configuration and possible candidates for flare trigger are briefly discussed with some SOT observations of solar flare events, which include X5.4/X1.3 flares on 7 March 2012, X1.2 flare on 7 January 2014 and two M-class flares on 2 February 2014. Especially, using an unique set of the Hinode and SDO data for the X5.4/X1.3 flares on 7 March 2012, we briefly reviewed remarkable properties observed in the spatial distribution of the photospheric magnetic flux, chromospheric flare ribbons, and the 3D coronal magnetic field structure inferred by non-linear force-free field modeling with the Hinode photospheric magnetic field data.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Ichimoto, K. et al. 2008, Solar Phys., 249, 233 Google Scholar
Inoue, S. et al. 2014, Astrophys. J., 780, 101 CrossRefGoogle Scholar
Kawabata, Y. 2016, Master thesis, The University of TokyoGoogle Scholar
Kosugi, T. et al. 2007, Solar Phys., 243, 3 Google Scholar
Lites, B. W. et al. 2013, Solar Phys., 283, 579 CrossRefGoogle Scholar
Shimizu, T. et al. 2008, Solar Phys., 249, 221 Google Scholar
Shimizu, T., Lites, B. W., & Bamba, Y. 2014, PASJ, 66 (SP1), S14 Google Scholar
Suematsu, Y. et al. 2008, Solar Phys., 249, 197 Google Scholar
Tsuneta, S. et al. 2008, Solar Phys., 249, 167 Google Scholar