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 models — Anthony Yeates¹, Tahar Amari², Ioannis Contopoulos^3,4, 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 Toeroek⁷ — ¹Durham 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.