Frontiers in Modeling Magnetic Flux Emergence and the Development of Solar Eruptive Activities Organizers: Mark Linton and Yuhong Fan SHINE Liaison: KD.

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Presentation transcript:

Frontiers in Modeling Magnetic Flux Emergence and the Development of Solar Eruptive Activities Organizers: Mark Linton and Yuhong Fan SHINE Liaison: KD Leka

Scene setting talks Mark Cheung: Physics and Diagnostics of the Drivers of Solar Eruptions James Leake: Developments in Model- Coupling for Simulations of Flux Emergence and Coronal Dynamics Discussion: How best to constrain E field driving condition? Cheung magnetofrictional example, current driving E has free parameter, setting this changes number of jets driven by E. Kazachenko talk (later) will describe constraining free parameter in E with Doppler measurements, etc. Titov poster: constrain E field driver with Lagrangian minimization method – to localize E and constrain to match Bz.

Discussion: Value of various diagnostic methods used in plasma physics, comparison of methods available in different fields. Solar physics: remote sensing – global picture, B field at photosphere plane (but not 3D B field). Cheung described new DEM weighted temperature diagnostic. Magnetospheric physics: in situ probes – can get close to reconnection region (MMS prospects) - but no remote sensing for context / large scale picture. Laboratory physics: Ha poster shows diagnostics for laboratory torus instability – combines remote sensing and in-situ. Also input current and inductance are well known: these represent global constraints on system.

Discussion: How high an error is acceptable in driving simulations with data? Leake test where ground truth known (previously run simulation): Magnetic energy errors around 10% (for small scale emergence event) when run at cadence of observed vector magnetograms from HMI. Acceptable: magnetograms themselves probably introduce a higher level of error. Unacceptable: free energy (excess above minimum for a particular boundary) may often be 10% of total in eruption / flare, so error at that level would change eruptivity. Discussion: Need to know thermodynamic variables as well? Likely important at photosphere, e.g., HMI data driving. Probably not important for magnetic field dynamics when model coupling is done at low Beta heights.