Evolution of Fine Structures in an Eruptive Active Region: Hinode (SOT/SP) Observations

Details Evolution of Fine Structures in an Eruptive Active Region: Hinode (SOT/SP) Observations Evolution of Fine Structures in an Eruptive Active Region: Hinode (SOT/SP) Observations

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh51a1268t&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH51A-1268

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere

Scientific paper

We study the evolution of an active region NOAA 10930 by using a large number of high resolution vector magnetograms obtained from Hinode (SOT/SP). A X3.4 class solar flare was observed from the active region NOAA 10930 (S06W35), which started at 02:14 UT on 13th December 2006. We have used HINODE (SOT/SP) data for 12, 13 and 14 December 2006 for studying spatial and temporal changes in pre and post eruption cases. The evolution of twist (computed from signed shear angle (SSA)) in the vector magnetograms is studied. It is known that the magnetic tension is reduced in highly sheared magnetic field regions e.g., polarity inversion lines. We study the evolution of magnetic tension near the polarity inversion line to check if the loss of magnetic tension was the possible cause of its eruption. We also study the evolution of AR NOAA 10961 as a non-erupting case. The difference between the evolution of fine structures in erupting and non-erupting active regions is the main motivation of this study.

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