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Solar MURI Vector Magnetogram Mini-Workshop

Solar MURI Vector Magnetogram Mini-Workshop. Using Vector Magnetograms in Theoretical Models: Plan of Action. Overview of the plan. Phase I Analyze available data for 1998 May 1 event Construct coronal magnetic equilibria Develop velocity inversion methods Test velocity inversion methods

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Solar MURI Vector Magnetogram Mini-Workshop

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  1. Solar MURI Vector Magnetogram Mini-Workshop Using Vector Magnetograms in Theoretical Models: Plan of Action MURI VMG mini-workshop

  2. Overview of the plan Phase I • Analyze available data for 1998 May 1 event • Construct coronal magnetic equilibria • Develop velocity inversion methods • Test velocity inversion methods • Study a second (simpler) event Phase II • Carry out MHD simulations • Couple coronal and IP codes Phase III • Validation of modelling using available solar and IP data MURI VMG mini-workshop

  3. Analyze available data for 1998 May 1 event • Generate a sequence of IVM magnetograms for the 1998 May 1 23:40 UT halo CME event (AR 8210), time cadence ~15 min (too slow ?), before, during, and after eruption. (Regnier) • Estimate the magnetic field uncertainties.(Metcalf, Leka) • Determine line of sight and transverse velocities. (Welsch, Metcalf) • Analyze the global solar (Li, Liu) and IP (Li, Luhmann) context (spatial, temporal) of this event, time scale ~ several days, including previous and following events. • Make an instrument vs time array on WWW (Li) MURI VMG mini-workshop

  4. Construct coronal magnetic equilibria • Build force-free magnetic field models for each magnetogram, combined with a potential extrapolation of MDI data. (Regnier) • Build magnetostatic models from the same magnetograms (Heinemann). • Compare force-free magnetic field models to available coronal imaging data (Canfield, Metcalf) • Compare connectivity of force-free models to that of point charge models (Regnier, Longcope, Leka) MURI VMG mini-workshop

  5. Develop velocity inversion methods • Use vertical component of induction equation to derive velocity fields (Longcope, Fisher, Welsch) • Constrain the solutions by minimizing total kinetic energy (ditto) MURI VMG mini-workshop

  6. Test velocity inversion methods • Generate fake magnetogram sequences from the MHD simulations (Abbett, Fisher) • Use velocity inversion techniques to infer velocities from these sequences (ditto + Welsch) • Compare photospheric boundary velocities from the simulation to those inferred from the inversion (same as 2) • Explore implications of magnetogram uncertainties through Monte Carlo methods (same as 2). • Compare velocities from the inversion to IVM observations (Welsch, Metcalf, Abbett, Fisher) MURI VMG mini-workshop

  7. Study a second (simpler) event (Liu) • Identify a simpler solar and IP event for analysis (1997 May 12 halo CME in AR8038 ?). • Produce a vector magnetogram (Solar Flare Telescope / Mitaka ?) sequence for this event. • Carry out an analysis parallel to that of the 1998 May 1 event (no velocity observations available – or use LCT methods for v_t, MDI for v_l?) (Liu + Welsch) MURI VMG mini-workshop

  8. Carry out MHD simulations • Do Zeus AMR simulations using real magnetic field data near time of CME using synoptic magnetic field solutions as boundary condition. (Berkeley mafia) • Couple coronal and interplanetary codes (Abbett, Ledvina, Odstrcil) MURI VMG mini-workshop

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