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Influence of non-potential coronal magnetic topology on solar wind models
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dc.contributor.author | Edwards, Sarah Jane | |
dc.contributor.author | Yeates, Anthony Robinson | |
dc.contributor.author | Bocquet, Francois | |
dc.contributor.author | Mackay, Duncan Hendry | |
dc.date.accessioned | 2016-10-28T23:34:00Z | |
dc.date.available | 2016-10-28T23:34:00Z | |
dc.date.issued | 2015-10 | |
dc.identifier | 223509487 | |
dc.identifier | 8f508707-a622-4723-bec3-6fa011ac407a | |
dc.identifier | 84947491423 | |
dc.identifier | 000365220000009 | |
dc.identifier.citation | Edwards , S J , Yeates , A R , Bocquet , F & Mackay , D H 2015 , ' Influence of non-potential coronal magnetic topology on solar wind models ' , Solar Physics , vol. 290 , no. 10 , pp. 2791-2808 . https://doi.org/10.1007/s11207-015-0795-8 | en |
dc.identifier.issn | 0038-0938 | |
dc.identifier.other | ORCID: /0000-0001-6065-8531/work/58055432 | |
dc.identifier.uri | https://hdl.handle.net/10023/9729 | |
dc.description.abstract | By comparing a magneto-frictional model of the low coronal magnetic field to a potential field source surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar wind speed solely from the magnetic field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar wind speed proxies. It contains twisted magnetic structures which can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher predicted wind speeds for two reasons: partly because magnetic flux tubes expand less rapidly with height, but more importantly because more open field lines are further from coronal hole boundaries. | |
dc.format.extent | 18 | |
dc.format.extent | 1811132 | |
dc.language.iso | eng | |
dc.relation.ispartof | Solar Physics | en |
dc.subject | Corona, models | en |
dc.subject | Magnetic fields, corona | en |
dc.subject | Magnetic fields, interplanetary | en |
dc.subject | Magnetic fields, models | en |
dc.subject | Solar wind, theory | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Influence of non-potential coronal magnetic topology on solar wind models | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. Applied Mathematics | en |
dc.identifier.doi | 10.1007/s11207-015-0795-8 | |
dc.description.status | Peer reviewed | en |
dc.date.embargoedUntil | 2016-10-28 | |
dc.identifier.url | http://link.springer.com/article/10.1007/s11207-015-0795-8 | en |
dc.identifier.grantnumber | ST/K000950/1 | en |
dc.identifier.grantnumber | PO: 4070103637 | en |
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