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  Global Non-Potential Magnetic Models of the Solar Corona During the March 2015 Eclipse

Yeates, A. R., Amari, T., Contopoulos, I., Feng, X., Mackay, D. H., Mikić, Z., et al. (2018). Global Non-Potential Magnetic Models of the Solar Corona During the March 2015 Eclipse. Space Science Reviews, 214: 99. doi:10.1007/s11214-018-0534-1.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0003-8E0B-2 Version Permalink: http://hdl.handle.net/21.11116/0000-0003-8E0F-E
Genre: Journal Article

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 Creators:
Yeates, Anthony R., Author
Amari, Tahar, Author
Contopoulos, Ioannis, Author
Feng, Xueshang, Author
Mackay, Duncan H., Author
Mikić, Zoran, Author
Wiegelmann, Thomas1, Author              
Hutton, Joseph, Author
Lowder, Christopher A., Author
Morgan, Huw, Author
Petrie, Gordon, Author
Rachmeler, Laurel A., Author
Upton, Lisa A., Author
Canou, Aurelien, Author
Chopin, Pierre, Author
Downs, Cooper, Author
Druckmüller, Miloslav, Author
Linker, Jon A., Author
Seaton, Daniel B., Author
Török, Tibor, Author
Affiliations:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              

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Free keywords: Magnetic fields Sun: surface magnetism Sun: corona
 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.

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Language(s): eng - English
 Dates: 2018
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Method: Peer
 Identifiers: DOI: 10.1007/s11214-018-0534-1
 Degree: -

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Title: Space Science Reviews
  Abbreviation : Space Sci Rev
Source Genre: Journal
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Publ. Info: Dordrecht : Springer Netherlands
Pages: - Volume / Issue: 214 Sequence Number: 99 Start / End Page: - Identifier: ISSN: 0038-6308
CoNE: https://pure.mpg.de/cone/journals/resource/954925446718