Will it Fit? A Comparison of Asymmetric Magnetic Reconnection Models and Observations Drake Ranquist...
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![Page 1: Will it Fit? A Comparison of Asymmetric Magnetic Reconnection Models and Observations Drake Ranquist Brigham Young University Advisors: Mari Paz Miralles.](https://reader036.fdocuments.us/reader036/viewer/2022062408/56649e9e5503460f94b9f838/html5/thumbnails/1.jpg)
Will it Fit?
A Comparison of Asymmetric Magnetic Reconnection Models
and Observations
Drake RanquistBrigham Young University
Advisors: Mari Paz Miralles and Nick Murphy2012 SAO Solar REU
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Magnetic ReconnectionOccurs in highly conducting
plasmas when magnetic fields are oriented in opposite directions
Observed in Plasma Experiments, Earth’s Magnetosphere, and the Sun’s Corona
Responsible for energy release and topology changes during solar eruptions
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Solar Flares and CMEsThe standard model of solar
eruptions includes:Rising plasmoid contained
by flux ropesX-line and current sheet
where magnetic reconnection occurs
Inflow and outflow at X-lineHot, bright post-flare loops
Locations where loops meet the photosphere are called footpoints
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NIMROD CodeStands for “Non-Ideal Magnetohydrodynamics with
Rotation and Other Doohickies”
Magnetohydrodynamics (MHD) describes macroscopic behavior of conducting fluids like plasmas using Maxwell’s equations and standard fluid hydrodynamics
Solutions represented as sums of finite element basis functions
Includes resistivity and anisotropic thermal conduction
Conducting wall boundary conditions that represent the photosphere
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Symmetrical Simulation
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Asymmetrical Simulation
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Observational Signatures of Asymmetric Reconnection
Distortion of post-flare loops
Asymmetric footpoint motions and brightness
Location of X-line and flow stagnation point
Different inflow velocities
Drifting of the CME current sheet
Circulation within the rising flux rope
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QuestionsCan we find evidence of asymmetric
reconnection in observations?
How well do the post-flare loops from the simulations agree with the observations?
Can we determine the ratio of magnetic field strengths on the two sides of an observed post-flare loop?
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Projection Effects:Symmetrical
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Projection Effects:Asymmetrical
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Observations: Two Events6/7 Dec 2010 and 7 Mar 2011
Primary Instruments:Atmospheric Imaging Assembly (AIA) on the Solar
Dynamics Observatory (SDO)SECCHI EUVI on STEREO-A and STEREO-B
Both events have a candle-like cusp at shorter wavelengths
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6/7 Dec 2010
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7 Mar 2011
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Tracing LoopsChoose loop to fit and trace it by clicking mouse
and saving X and Y coordinates
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Matching SimulationsWe assumed that the footpoints of the trace and
the simulation had to be at the same locationMagnetic field lines tied to solar surface Important to know exact location of footpointsCan automatically scale, center, and rotate
simulation about the Z axis
Only free parameters are:Rotation about the baselineLoop heightMagnetic field asymmetry
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2010 Event
Symmetric Case Asymmetric Case
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2011 Event
Symmetric Case Asymmetric Case
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Results (AIA Only)Event 2010
12 loops traced8 loops match
simulations8:1 – 5 loops4:1 – 2 loops2:1 – 1 loop
Event 20117 loops traced6 loops match
simulations4:1 – 3 loops2:1 – 1 loop1.5:1 – 1 loop1.25:1 – 1 loop
These are the best fits in the AIA data, but not the only possible fits. Rotation into STEREO further constrained
results.
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Rotation To Stereo
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ProblemsSimulations are Two Dimensional
Doesn’t allow for more complicated 3-D structure
Simulated loops are isolated
Difficult to trace loopsThey split, merge, and twist
Footpoints often saturated giving greater error to location
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ConclusionsThe simulations are able to fit most observations
This technique can be used to get a rough estimate on magnetic field asymmetries
The 6/7 Dec 2010 event is consistent with a magnetic field asymmetry of 4:1
The 7 Mar 2011 event is consistent with a magnetic field asymmetry of around 1.5:1
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Future WorkUse same process for other events
See if HMI Magnetograms and potential field models indicate similar asymmetries
Determine error on tracing loops (especially with the footpoint locations)
Look for other observational signatures of asymmetrical reconnection and compare them to these results.
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AcknowledgementsAdvisors Mari Paz Miralles and Nick Murphy
Harvard-Smithsonian Solar REU Program
NSF Grant that supports the REU ProgramATM-0851866
Ed DeLuca, Kathy Reeves, EMS crew, Hospital Staff, my Parents, and everyone else that kept me alive
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Loop Unable to Fit (Kink)
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HMI Magnetograms6 Dec 2010 7 Mar 2011