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Modeling the sun's small-scale global photospheric magnetic field
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dc.contributor.author | Meyer, Karen Alison | |
dc.contributor.author | Mackay, Duncan Hendry | |
dc.date.accessioned | 2016-09-15T15:30:10Z | |
dc.date.available | 2016-09-15T15:30:10Z | |
dc.date.issued | 2016-10-19 | |
dc.identifier | 244441613 | |
dc.identifier | 2aae8b18-67fd-42d8-8b64-68fce3bc9c40 | |
dc.identifier | 84992744455 | |
dc.identifier | 000386583400012 | |
dc.identifier.citation | Meyer , 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/830/2/160 | en |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | ORCID: /0000-0001-6065-8531/work/58055457 | |
dc.identifier.uri | https://hdl.handle.net/10023/9511 | |
dc.description.abstract | We 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.extent | 13 | |
dc.format.extent | 4782187 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astrophysical Journal | en |
dc.subject | Sun: activity | en |
dc.subject | Sun: corona | en |
dc.subject | Sun: magnetic fields | en |
dc.subject | Sun: photosphere | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | NDAS | en |
dc.subject | BDC | en |
dc.subject | R2C | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Modeling the sun's small-scale global photospheric magnetic field | en |
dc.type | Journal article | en |
dc.contributor.sponsor | The Leverhulme Trust | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | EPSRC | en |
dc.contributor.institution | University of St Andrews. Applied Mathematics | en |
dc.identifier.doi | 10.3847/0004-637X/830/2/160 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | RPG-305 | en |
dc.identifier.grantnumber | ST/K000950/1 | en |
dc.identifier.grantnumber | ST/N000609/1 | en |
dc.identifier.grantnumber | N/A | en |
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