summary of ucb muri workshop on vector magnetograms
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Summary of UCB MURI workshop on vector magnetograms. Have picked 2 observed events for targeted study and modeling: AR8210 (May 1, 1998), and AR8038 (May 12, 1997) - PowerPoint PPT PresentationTRANSCRIPT
Summary of UCB MURI workshop on vector magnetograms
• Have picked 2 observed events for targeted study and modeling: AR8210 (May 1, 1998), and AR8038 (May 12, 1997)
• “Plan of Action” formulated (see http://solarmuri.ssl.berkeley.edu/~fisher/public/presentations/vmgram-workshop-2002/ . for details
• Have started modeling AR8210 – It is difficult! Challenges: Generating initial conditions self-consistently, deriving physically consistent velocity fields at photosphere, real versus numerical time scales
MDI magnetogram of AR8210
This active region was extremely well observed, was responsible for a number of flares and CMEs, and has a
fascinating evolution across the solar disk…
First step: Drive MHD model with “fake” data of flux emergence from another MHD
simulation
• Tests ability to drive an MHD calculation from boundary
• Boundary values of variables guaranteed to be physically consistent
Test calculations of flux emergence and comparisons with potential field models
Velocities: Why it is essential to know them:
• Physically consistent evolution at bottom plane in a simulation:
Terms on LHS describe evolution driven by horizontal motion; RHS describes evolution due to flux emergence or submergence
• This requires knowledge of vector components of B and v.
• How do we determine v self-consistently from a sequence of vector magnetograms?
• Price for ignoring the problem: Incorrect coronal magnetic topology
)()(
Bv zzt
vBBz
We are exploring several methods for finding the velocity of magnetized plasma:
• Stokes Profiles could be used to get vz
• Local Correlation Tracking (LCT) can find a velocity field v (But is it correct?)
• Vertical component of induction equation provides a constraint equation on v from a sequence of vector magnetograms (but solution is under-constrained)
• Kusano et al. used combination of LCT and vertical induction equation to solve for vz
• Longcope has developed a solution by adding an additional constraint: minimize the horizonal kinetic energy. Method appears to work in some cases, but not yet thoroughly tested.
LCT tests show it works some times and not others…
Apply a velocity field to an image consisting of random hash – can LCT correctly recover the velocity?
Recovered velocity fields…
Here, it did correctly find the applied horizontal velocity field…
Vx Vy
Here it doesn’t work so well:
2 images of Bz taken at a horizontal plane of one of Bill Abbett’s flux emergence simulations:
Comparison of LCT and actual horizontal velocity fields:
Note LCT velocity is very wrong in the outer regions…
actual LCT
This illustrates some serious shortcomings to LCT:
• In order for local correlation tracking to work, there must be some “structure” in the image
• There is (at least one) arbitrary constant (e.g. the “tile size”) which must be specified a-priori
• LCT cannot give any information about vertical velocities
• LCT will incorrectly determine the horizontal velocity when magnetic flux is emerging or submerging
Try an alternative approach based on ideal MHD induction equation applied at boundary plane:
• Magnetic quantities known from sequence of vector magnetograms
• This equation provides an (underdetermined) constraint on the velocity field. With additional assumptions, a physically consistent velocity field can be found.
• Details of Longcope’s proposed solution available at http://solarmuri.ssl.berkeley.edu/~dana/public/presentations/
)()(
Bv zz
z vBt
B
Result of applying Dana’s method to AR8210:
And so what happens in MHD simulations of AR8210?
• Stay tuned! Simulations are running even as we speak….