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Vincent Surges
Advisors:Yingna Su
Aad van Ballegooijen
Observations and Magnetic Field Modeling of a
flare/CME event on 2010 April 8
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Solar Eruptions include…
• Coronal Mass Ejections (CME)
• Prominence Eruptions
• Solar Flares
Notable Common Features
-Often occur in the Sun’s active regions
-All involve sudden release of massive energy
-All powered by same physical process
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Magnetic Reconnection
In Solar EruptionsStressed coronal magnetic field
Relieved by restructuring field lines
= lower energy
Previously trapped energy converted:
• kinetic
• thermal
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Motivation for research
Why study solar eruptions?
-Impact on space weather
-Potentially dangerous:
• Emits energy/radiation
• Problems on Earth
• Dangers in space
Active area of research!
Overview of My Project• Modeling flare/CME event in AR 11060
from 2010 April 8 at ~02:30 UT
• Two models created
1) best-fit NLFFF model prior to eruption
• Accomplished using Coronal Modeling System (CMS) to match coronal loops with created field lines
2) Unstable model of magnetic field during event onset
• Compared with flare footpoints and ribbons at event onset
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Instruments
Solar Dynamics Observatory
• Atmospheric Imaging Assembly (AIA) 7 EUV and 3 UV-visible channels Four telescopes
• Helioseismic and Magnetic Imager (HMI) Measures magnetic field strength in
photosphere
Hinode
• X-Ray Telescope (XRT) Soft X-ray images reveal magnetic field
configuration Observe the energy buildup, storage,
and release process in the corona
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AIA 193
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MHD and Nonlinear Force-Free Fields
Equation of Motion:
In static equilibrium:
Force-Free condition:
One Solution
Assume (current free)
Potential field:
No free magnetic energy in potential field!
Potential field does not match observations
Different solution
Assume
Nonpotential field:
Free energy = nonpotential - potential
in a nonpotential field:
- Constant along field lines
1) α=0 Potential Field
2) α=constant Linear Force-Free Field
3) α=α(r) Nonlinear Force-Free Field (NLFFF)
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Creating NLFFF models using CMS
Flux Rope Insertion Method• Construct potential field of region• Create cavity - Insert bundle along path• Two parameters: Poloidal = twist
Axial = shear
• Allow flux rope to relax
Magneto-frictional Relaxation
-Expands flux rope using artificial friction
Two Possibilities-
1) Flux rope reaches equilibrium
2) Flux rope erupts as flare/CME
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Five Models After Relaxation
• Step 1: Find threshold
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Five Models After Relaxation
• Step 1: Find threshold
• Threshold:
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Observing Coronal Loops
• Step 2: Locate observed loops
Loop 1 from AIA 171
Loop 2 from AIA 193
(plotted on AIA 171)
Loops 3, 4, 5 from XRT
• •
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Finding Best-Fit Model
Step 3: Analyzing Comparisons Model must fit observed loops Expect to be stable ( )
Did not use since value >> threshold
Loop 1 Loop 2 Loop 3 Loop 4 Loop 5
0.0032 0.0029 0.0035 0.0014 0.0033
0.0024 0.0027 0.0007 0.0003 0.0011
0.0022 0.0041 0.0004* 0.0011 0.0004
0.0026* 0.0082 0.0005* 0.0029 0.0006
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Best Model Prior to Eruption
Observing best-fit model:
• Modeled field lines extend higher in (b) due to shorter observed loops• Closely matched observed loops + low AD value = Excellent model
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Unstable Model
Model 2:
• Flux rope continues expanding during relaxation
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Different Segments of Flux Rope
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Summary/Future Work
Our best-fit pre-flare NLFFF ( ) contains a highly sheared and weakly twisted flux rope.
The axial flux in the pre-flare model is close to the threshold ( ).
The unstable model ( ) matches the observations at the early phase of the flare.
All these results strongly support that this event is due to the loss-of-equilibrium mechanism.
Use the unstable model as initial conditions for full 3D-MHD simulations of the observed CME event.
Applying this method to more events.
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A Special Thanks
to
Dr. Yingna Su
Dr. Aad van Ballegooijen
Solar Stellar X-Ray Group
Harvard-Smithsonian Center for Astrophysics National Science Foundation