Observations and Magnetic Field Modeling of the Solar Flare/CME Event on 2010 April 8

Su Yingna, ynsu@head.cfa.harvard.edu, Harvard-Smithsonian Center for Astrophysics, United States
Kliem Bernhard, Institute for Physics and Astronomy, University, Potsdam
van Ballegooijen Adriaan, Harvard-Smithsonian Center for Astrophysics
Surges Vicent, Harvard-Smithsonian Center for Astrophysics
Deluca Edward, Harvard-Smithsonian Center for Astrophysics
Golub Leon, Harvard-Smithsonian Center for Astrophysics

Abstract
We present two studies 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. The CME is observed by STEREO and SOHO/LASCO. We create a series of static magnetic field models, using the flux-rope insertion method developed by van Ballegooijen (2004). The boundary conditions for the magnetic fields are provided by line-of-sight magnetograms taken by SDO/HMI. The best-fit NLFFF model is constrained by the coronal loops observed by SDO/AIA and Hinode/XRT. We find that the axial flux in the best-fit pre-flare NLFFF model (Axi=4e20 Mx) is close to the threshold of instability (Axi=5e20 Mx). The unstable model (Axi=6e20 Mx) matches the flare footpoints and coronal dimmings as observed at the early phase of the event. We also produce scaled versions of these three models in Cartesian geometry, and use these models as realistic initial conditions for three-dimensional zero-beta MHD simulations (Torok & Kliem 2003, Kliem et al. 2004). These MHD simulations confirm that the model with axial flux of 4e20 Mx is stable, while the model with axial flux of 6e20 Mx erupts as a real CME. Detailed comparisons of the CME model with observations (e.g, dynamics, morphology, erupting direction of the CME) will be presented.