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

Observations and Magnetic Field Modeling of the Flare/CME Event on 2010 April 8. Yingna Su Bernhard Kliem , Adriaan van Ballegooijen , Vincent Surges, Edward Deluca. Presentation at Hinode-5 on Oct 13, 2011, Cambridge, USA. Overview.

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

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  1. Observations and Magnetic Field Modeling of the Flare/CME Event on 2010 April 8 Yingna Su Bernhard Kliem, Adriaan van Ballegooijen, Vincent Surges, Edward Deluca Presentation at Hinode-5 on Oct 13, 2011, Cambridge, USA

  2. Overview Part I: We construct static magnetic field models using the flux rope insertion method to compare with observations prior to and at the onset of the event. (Su et al. 2011, ApJ, 734, 53) Part II: We conduct zero-beta MHD simulations using the aforementioned models as initial conditions to compare with the dynamics of the event. (Kliem et al. 2011, in preparation)

  3. Observations of the Event

  4. Observations before the Event

  5. Part I

  6. Flux Rope Insertion Method • Construct potential field model using a line-of-sight magnetogram. • Create a cavity, then insert a magnetic flux bundle along the selected filament path. • Allow the fields to relax using magneto-frictional relaxation, which leads to two possibilities: 1) The configuration reaches an equilibrium --NLFFF model. 2) The configuration erupts as a flare/CME – Unstable model.

  7. Stability of the Model • Panels b-c: Stable; Panel d: Marginally Stable; Panels e-f: Unstable

  8. Pre-flare NLFFF Model • The two free parameter, i.e., poloidal flux (twist) and axial flux (shear), are constrained by the observed non-potential loops. • The best-fit pre-flare model: axial flux =4e20 Mx, poloidal flux=1e10 Mx/cm. It contains a highly sheared and weakly twisted flux rope.

  9. Models at the Event Onset • The unstable model (axi=6e20Mx, pol=1e20 Mx/cm) due to increase of axial flux closely matches the observations at the event onset. • The aixal flux (4e20 Mx) in the best-fit pre-flare model is close to the threshold of instability (5e20 Mx).

  10. Models at the Event Onset • The unstable model (axi=4e20 Mx, pol=30e10 Mx/cm) due to increase of poloidal flux (twist) does not match the observations. • The poloidal flux (1e10 Mx/cm) in the best-fit pre-flare model is far away from the threshold of instability (30e10 Mx/cm).

  11. Part II

  12. Method • Zero-beta MHD simulations using the static models constructed in Part I as initial conditions. Remove the flux imbalance Static Model --------------------------------- MHD simulation Coordinate conversion Spherical Coordinate HIRES region: 43 (lon)x39(lat) Resolution: 0.002Rsun Domain: extends to 2Rsun Cartesian Coordinate Closed top and side boundaries Fixed bottom b.c. No B smoothing Viscosity =0.002

  13. Stable Model

  14. Marginally Stable Model

  15. Unstable Model

  16. Unstable Model

  17. Observation vs. Model

  18. Observation vs. Model

  19. Summary • Our best-fit pre-flare NLFFF model (Axi=4e20 Mx, Pol=1e10 Mx/cm) contains a highly sheared and weakly twisted flux rope (Figure 2b). • The axial flux of the flux rope in the best-fit pre-flare model is close to the threshold of instability (Axi=5e20 Mx). • The unstable model (Axi=6e20 Mx, Pol=1e10 Mx/cm) matches the observations at the early phase of the flare. • All these results strongly support that this event may be due to the loss-of-equilibrium mechanism. • As a following step, we will try to find the threshold of the poloidal flux of the flux rope for a fixed axial flux (4e20 Mx/cm). • The unstable model can be used as initial conditions for full 3D-MHD simulations of the observed CME event.

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