Observations and Magnetic Field Modeling of CMEs’ Source Regions Yingna Su Harvard-Smithsonian Center for Astrophysics Collaborators: Adriaan van Ballegooijen,

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Observations and Magnetic Field Modeling of CMEs’ Source Regions Yingna Su Harvard-Smithsonian Center for Astrophysics Collaborators: Adriaan van Ballegooijen, Bernhard Kliem, Vincent Surges, Edward Deluca, Leon Golub Presentation at the NESSC Meeting on Oct 24, 2012, UNH, New Hampshire

Overview Part I: Observations and modeling (Static and MHD) of an active region flare/CME event. (Su et al. 2011, ApJ, 734, 53; Su et al. 2012, IAUs 294 submitted) Part II: Observations and modeling of one eruptive polar crown prominence (Su et al. 2012b, ApJ, in preparation)

Part I: Observations and modeling (Static and MHD) of an active region flare/CME event. (Su et al. 2011, ApJ, 734, 53; Su et al. 2012, IAUs 294 submitted)

Observations of the Flare/CME Event Time: 02:30 UT on Apr. 8, 2010 Location: AR (N25E16) GOES B3.7 flare CME: V=174km/s Dimmings SDO/AIA 193

Observations before the Event  Two sets of loops  Two filaments  Flux cancellations along the PIL

Flux Rope Insertion Method Construct potential field model using an observed 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.

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

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.

Model at the Event Onset The unstable model (axi=6e20Mx, pol=1e10 Mx/cm) due to increase of axial flux closely matches the observations at the event onset. The axial flux (4e20 Mx) in the best-fit pre-flare model is close to the threshold of instability (5e20 Mx).

Zero-beta MHD Simulations Axi=4e20 Mx Pol=1e10 Mx/cm Axi=6e20 Mx Pol=1e10 Mx/cm Axi=6e20 Mx Pol=1e10 Mx/cm Stable Model Unstable Model

Summary I  Our best-fit pre-flare NLFFF model (Axi=4e20 Mx, Pol=1e10 Mx/cm) contains a highly sheared and weakly twisted flux rope.  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) due to increase of axial flux closely 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, which is caused by an increase of axial flux driven by the flux cancellations.  Using the aforementioned static models as initial conditions, the full 3D-MHD simulations confirm the statements that the best-fit flare model is stable, and the unstable model with axial flux of 6e20 Mx leads to a CME.  To Do: Further detailed comparisons of the CME observations and simulations.

Part II: Observations and modeling of one eruptive polar crown prominence (Su et al. 2012b, ApJ, in preparaition)

Polar Crown Prominence Eruption  On 2010 December 6 around 14:16 UT, filament in the active region core breaks apart.  Eruption of the quiescent filament  Eruption of the elevated active region filament  Several segments of the filament  CME speed: ~523 km/s

Rolling Motion: STEREO_B vs. Model  Observation: clockwise rolling motion around the filament axis  Model: Additional twist is injected to the flux rope from the west. Prominence: discrete blobs---field lines---helical flux rope Motion of blobs: equation of motion (gravity and friction)

Asymmetric Current distribution

Asymmetric Reconnection Murphy et al. 2012

Rotating Motion: SDO vs. Model  Observations: rotational motion of vertical threads while falling down.  Model: removal of dips in the field lines from top down.

Summary II  Sideway eruption: begins in the active region core, then quiescent filament erupts, which is followed by the eruption of the AR filament.  The observed rolling motion around the filament axis is reproduced in our 3D model, which suggests twist injection. Kink instability?  The rolling motion may be caused by asymmetric reconnection.  Our model reproduced the observed rotational motion, which suggests removal of field line dips from top down.

Thank you!

MHD Simulations 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 Cartesian Coordinate Domain:.72x.72x1 Rsun (41x41 degrees) Closed top and side boundaries Bz=const & U=0 in z=0 [Numerical diffusion params close to lower limits for num. stab.] Spherical Coordinate HIRES region: 43 (lon)x39(lat) Resolution: 0.002Rsun Domain: extends to 1Rsun Side boundaries: Bn=0 Top boundaries: open field Scaling factor: 1/16.97

Position-time plot

Observations vs. Unstable Model