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dc.contributor.authorMeyer, Karen Alison
dc.contributor.authorMackay, Duncan Hendry
dc.date.accessioned2016-09-15T15:30:10Z
dc.date.available2016-09-15T15:30:10Z
dc.date.issued2016-10-19
dc.identifier244441613
dc.identifier2aae8b18-67fd-42d8-8b64-68fce3bc9c40
dc.identifier84992744455
dc.identifier000386583400012
dc.identifier.citationMeyer , K A & Mackay , D H 2016 , ' Modeling the sun's small-scale global photospheric magnetic field ' , Astrophysical Journal , vol. 830 , no. 2 , 160 , pp. 1-13 . https://doi.org/10.3847/0004-637X/830/2/160en
dc.identifier.issn0004-637X
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055457
dc.identifier.urihttps://hdl.handle.net/10023/9511
dc.description.abstractWe present a new model for the Sun's global photospheric magnetic field during a deep minimum of activity, in which no active regions emerge. The emergence and subsequent evolution of small-scale magnetic features across the full solar surface is simulated, subject to the influence of a global supergranular flow pattern. Visually, the resulting simulated magnetograms reproduce the typical structure and scale observed in quiet Sun magnetograms. Quantitatively, the simulation quickly reaches a steady state, resulting in a mean field and flux distribution that are in good agreement with those determined from observations. A potential coronal magnetic field is extrapolated from the simulated full Sun magnetograms to consider the implications of such a quiet photospheric magnetic field on the corona and inner heliosphere. The bulk of the coronal magnetic field closes very low down, in short connections between small-scale features in the simulated magnetic network. Just 0.1% of the photospheric magnetic flux is found to be open at 2.5 R⊙, around 10–100 times less than that determined for typical Helioseismic and Magnetic Imager synoptic map observations. If such conditions were to exist on the Sun, this would lead to a significantly weaker interplanetary magnetic field than is currently observed, and hence a much higher cosmic ray flux at Earth.
dc.format.extent13
dc.format.extent4782187
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectSun: activityen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: photosphereen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleModeling the sun's small-scale global photospheric magnetic fielden
dc.typeJournal articleen
dc.contributor.sponsorThe Leverhulme Trusten
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEPSRCen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doi10.3847/0004-637X/830/2/160
dc.description.statusPeer revieweden
dc.identifier.grantnumberRPG-305en
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumberST/N000609/1en
dc.identifier.grantnumberN/Aen


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