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Title:
Observations and Nonlinear Force-Free Field Modeling of Active Region 10953
Authors:
Su, Yingna; van Ballegooijen, Adriaan; Lites, Bruce W.; Deluca, Edward E.; Golub, Leon; Grigis, Paolo C.; Huang, Guangli; Ji, Haisheng
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ; Purple Mountain Observatory, Nanjing, 210008, China ; ), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ), AC(High Altitude Observatory, P.O. Box 3000, Boulder, CO 80307-3000, USA), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ), AG(Purple Mountain Observatory, Nanjing, 210008, China ), AH(Purple Mountain Observatory, Nanjing, 210008, China )
Publication:
The Astrophysical Journal, Volume 691, Issue 1, pp. 105-114 (2009). (ApJ Homepage)
Publication Date:
01/2009
Origin:
IOP
ApJ Keywords:
Sun: corona, Sun: filaments, Sun: flares, Sun: magnetic fields, Sun: photosphere, Sun: X-rays, gamma rays
DOI:
10.1088/0004-637X/691/1/105
Bibliographic Code:
2009ApJ...691..105S

Abstract

We present multiwavelength observations of a simple bipolar active region (NOAA 10953), which produced several small flares (mostly B class and one C8.5 class) and filament activations from April 30 to May 3 in 2007. We also explore nonlinear force-free field (NLFFF) modeling of this region prior to the C8.5 flare on May 2, using magnetograph data from SOHO/MDI and Hinode/SOT. A series of NLFFF models are constructed using the flux-rope insertion method. By comparing the modeled field lines with multiple X-ray loops observed by Hinode/XRT, we find that the axial flux of the flux rope in the best-fit models is (7± 2)× 1020 Mx, while the poloidal flux has a wider range of (0.1-10)× 1010 Mx cm-1. The axial flux in the best-fit model is well below the upper limit (~15× 1020 Mx) for stable force-free configurations, which is consistent with the fact that no successful full filament eruption occurred in this active region. From multiwavelength observations of the C8.5 flare, we find that the X-ray brightenings (in both RHESSI and XRT) appeared about 20 minutes earlier than the EUV brightenings seen in TRACE 171 Å images and filament activations seen in MLSO Hα images. This is interpreted as an indication that the X-ray emission may be caused by direct coronal heating due to reconnection, and the energy transported down to the chromosphere may be too low to produce EUV brightenings. This flare started from nearly unsheared flare loop, unlike most two-ribbon flares that begin with highly sheared footpoint brightenings. By comparing with our NLFFF model, we find that the early flare loop is located above the flux rope that has a sharp boundary. We suggest that this flare started near the outer edge of the flux rope, not at the inner side or at the bottom as in the standard two-ribbon flare model.
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