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dc.contributor.authorEdwards, Sarah Jane
dc.contributor.authorYeates, Anthony Robinson
dc.contributor.authorBocquet, Francois
dc.contributor.authorMackay, Duncan Hendry
dc.identifier.citationEdwards , 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 .
dc.identifier.otherPURE: 223509487
dc.identifier.otherPURE UUID: 8f508707-a622-4723-bec3-6fa011ac407a
dc.identifier.otherScopus: 84947491423
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055432
dc.identifier.otherWOS: 000365220000009
dc.description.abstractBy 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.relation.ispartofSolar Physicsen
dc.rights© 2015, Publisher / the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at /
dc.subjectCorona, modelsen
dc.subjectMagnetic fields, coronaen
dc.subjectMagnetic fields, interplanetaryen
dc.subjectMagnetic fields, modelsen
dc.subjectSolar wind, theoryen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleInfluence of non-potential coronal magnetic topology on solar wind modelsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden
dc.identifier.grantnumberPO: 4070103637en

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