Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11a1613s&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH11A-1613
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions
Scientific paper
We present a study on the flare/CME event that occurred in Active Region 11060 on 2010 April 8. This flare is well observed at multiple EUV and UV channels by SDO/AIA. This flare is a typical two-ribbon flare associated with both coronal dimming and wave, the associated CME is observed by STEREO and SOHO/LASCO. Using the flux-rope insertion method developed by van Ballegooijen (2004), two magnetic field models of the active region are created: (1) best-fit nonlinear force-free field model (NLFFF) of the region prior to the eruption; (2) unstable state of the magnetic fields present at the onset of the event. The boundary conditions of the magnetic fields are provided by the LOS magnetograms taken by SDO/HMI. The best-fit NLFFF model is constrained by the coronal loops observed by SDO/AIA and Hinode/XRT. The best-fit model prior to the flare contains a highly sheared and weakly twisted flux rope. The axial flux of the flux rope in this model is very close to the threshold of instability. The location of the flare ribbons and flare loops at the event onset closely match the reconnected field lines from the unstable model. The footpoints of the erupting flux rope are located near the coronal dimming region. These results suggest that this event may be due to the loss-of-equilibrium mechanism. The unstable model can also be used as initial condition for full 3D-MHD simulations of the observed CME event.
Su Yuehua
Surges Vincent
van Ballegooijen Adriaan A.
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