Global Non-Potential Magnetic Models of the Solar Corona During the March 2015 Eclipse |
| |
| Authors: | Anthony R Yeates Tahar Amari Ioannis Contopoulos Xueshang Feng Duncan H Mackay Zoran Mikić Thomas Wiegelmann Joseph Hutton Christopher A Lowder Huw Morgan Gordon Petrie Laurel A Rachmeler Lisa A Upton Aurelien Canou Pierre Chopin Cooper Downs Miloslav Druckmüller Jon A Linker Daniel B Seaton Tibor Török |
| |
| Institution: | 1.Department of Mathematical Sciences,Durham University, Science Laboratories,Durham,UK;2.CNRS,Centre de Physique Théorique de l’Ecole Polytechnique,Palaiseau Cedex,France;3.Research Center for Astronomy and Applied Mathematics,Academy of Athens,Athens,Greece;4.National Research Nuclear University (MEPhI),Moscow,Russia;5.State Key Laboratory of Space Weather, National Space Science Center,Chinese Academy of Sciences,Beijing,China;6.School of Mathematics and Statistics,University of St Andrews,St Andrews,UK;7.Predictive Science, Inc.,San Diego,USA;8.Max-Planck Institut für Sonnensystemforschung,G?ttingen,Germany;9.Institute of Mathematics, Physics & Computer Sciences,Aberystwyth University,Aberystwyth,UK;10.Southwest Research Institute,Boulder,USA;11.National Solar Observatory,Boulder,USA;12.NASA Marshall Space Flight Center,Huntsville,USA;13.High Altitude Observatory,National Center for Atmospheric Research,Boulder,USA;14.Faculty of Mechanical Engineering,Brno University of Technology,Brno,Czech Republic;15.Cooperative Institute for Research in Environmental Sciences,University of Colorado,Boulder,USA;16.National Centers for Environmental Information,National Oceanic and Atmospheric Administration,Boulder,USA |
| |
| Abstract: | Seven different models are applied to the same problem of simulating the Sun’s coronal magnetic field during the solar eclipse on 2015 March 20. All of the models are non-potential, allowing for free magnetic energy, but the associated electric currents are developed in significantly different ways. This is not a direct comparison of the coronal modelling techniques, in that the different models also use different photospheric boundary conditions, reflecting the range of approaches currently used in the community. Despite the significant differences, the results show broad agreement in the overall magnetic topology. Among those models with significant volume currents in much of the corona, there is general agreement that the ratio of total to potential magnetic energy should be approximately 1.4. However, there are significant differences in the electric current distributions; while static extrapolations are best able to reproduce active regions, they are unable to recover sheared magnetic fields in filament channels using currently available vector magnetogram data. By contrast, time-evolving simulations can recover the filament channel fields at the expense of not matching the observed vector magnetic fields within active regions. We suggest that, at present, the best approach may be a hybrid model using static extrapolations but with additional energization informed by simplified evolution models. This is demonstrated by one of the models. |
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
