Physics
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1921l&link_type=abstract
American Astronomical Society, SPD meeting #40, #19.21; Bulletin of the American Astronomical Society, Vol. 41, p.850
Physics
Scientific paper
Recent observations demonstrated the rapid penumbra decay in the outer δ-sunspot and the enhancement of inner penumbrae and central umbrae after major flares. In an effort to understand the physics behind the phenomena, we study the changes of magnetic inclination angle at the peripheral and the inner penumbral regions around the time of three X-class flares, the X3.4 flare on 2006 December 13, the X2.6 flare on 2005 January 15 and the X5.3 flare on 2001 August 25. For the first event, we use the Hinode Spectro-Polarimeter (SP) vector magnetograms before and after the flare, between which there was an 8-hour interval. For the two latter events, the high cadence vector magnetograms obtained with the Digital Vector Magnetograph (DVMG) at Big Bear Solar Observatory (BBSO) are available, with which we are able to study the inclination angle as a function of time. For all the events, we find that the mean inclination angle at the penumbral decay regions increases after flares. The result suggests that penumbral fields change from a more inclined to a more vertical configuration after the flare. Furthermore, we derive the three-dimensional coronal magnetic fields using nonlinear force-free field extrapolation to study the altitude variation of magnetic inclination angle.
Jing Ji-liang
Li Yixuan
Wang Hai-Hong
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