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Verhandlungen
Verhandlungen
DPG

Würzburg 2018 – scientific programme

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EP: Fachverband Extraterrestrische Physik

EP 3: Sun and Heliosphere I - Structure (MHD, Corona, TR, SW-acc.-Region)

EP 3.2: Talk

Tuesday, March 20, 2018, 17:00–17:15, BSZ - Pabel HS

Global non-potential coronal magnetic field modelsAnthony Yeates1, Tahar Amari2, Ioannis Contopoulos3,4, Xueshang Feng5, Duncan Mackay6, Zoran Mikic7, •Thomas Wiegelmann8, Joseph Hutton9, Christopher Lowder1, Huw Morgan9, Gordon Petrie10, Laurel Rachmeler11, Lisa Upton12, Aurelien Canou2, Pierre Chopin2, Cooper Downs7, Miloslav Druckmueller13, John Linker7, Daniel Seaton14, and Tibor Toeroek71Durham University — 2CNRS, Paris — 3Research Center for Astronomy, Athens — 4MEPhl, Moscow — 5National Space Science Center, Beijing — 6University of St. Andrews — 7Predictive Science, San Diego — 8MPI for Solar-Sytem-Research, Goettingen — 9Institute of Mathematics and Physics, Aberystwyth — 10NSO, Boulder — 11NASA Marshal Space Flight Center, Huntsville — 12High Altitude Observatory, Boulder — 13Brno University of Technology — 14Royal Observatory of Belgium

Within an international collaboration we compared several static and evolutionary global corona models: non-linear force-free, magneto-static, evolutionary magneto-frictional, full MHD and zero-beta MHD. The models agree on the amount of open flux, streamer location and broad magnetic topology. They disagree on the shape of helmet streamers and electric currents. Static models are better in active regions, evolutionary models better to model filaments. Our advise is to combine static extrapolations with energysation from evolutionary models.

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