| Magnetic Field EvolutionÉ |
| Two different theoretical studies of magnetic field evolution |
| First Approach: Exploration Ð this is how most research in Solar Physics is done today |
| Second Approach: ÒPrognosticÓ Modeling |
| Slide 5 |
| The Transport of Magnetic Flux |
| Slide 7 |
| The Turbulent Dynamo |
| Slide 9 |
| Slide 10 |
| The Turbulent Dynamo and X-ray Flux in Stars |
| The Turbulent Dynamo and X-ray Flux in Stars |
| Can we develop a physics-based model of magnetic field evolution that could predict solar flares and coronal mass ejections? |
To what extent can we determine the flows in an active region by observing changes in the magnetic field at the photosphere? |
| Determining the physically consistent flow field is an essential part of this problem |
| The LCT, FLCT techniques |
| Example of FLCT applied to NOAA AR 8210 (May 1 1998) |
| The Demoulin & Berger Interpretation of LCT |
| The Ideal MHD Induction Equation |
| ILCT Ð Use LCT to constrain solutions of the induction equation |
| Apply ILCT to IVM vector magnetogram data for AR 8210 |
| Must have some kind of initial conditions: |
| Time dependent boundary conditions for the coronal MHD code |
| Illustration of 2 coupled codes |
| Toward a Data-driven
Simulation of AR-8210 4 hrs of solar time, corresponding to the vector magnetogram time sequence |
| Data Driven
Simulations: Plans for future |