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dc.contributor.authorPriest, Eric
dc.date.accessioned2017-07-28T14:30:10Z
dc.date.available2017-07-28T14:30:10Z
dc.date.issued2017-07-14
dc.identifier.citationPriest , E 2017 , ' Our dynamic sun : 2017 Hannes Alfvén Medal lecture at the EGU ' , Annales Geophysicae , vol. 35 , pp. 805-816 . https://doi.org/10.5194/angeo-35-805-2017en
dc.identifier.issn0992-7689
dc.identifier.otherPURE: 250573005
dc.identifier.otherPURE UUID: f6fda07b-d73a-458c-abcb-3b48229bd838
dc.identifier.otherScopus: 85024384802
dc.identifier.otherWOS: 000406342300001
dc.identifier.urihttp://hdl.handle.net/10023/11320
dc.description.abstractThis lecture summarises how our understanding of many aspects of the Sun has been revolutionised over the past few years by new observations and models. Much of the dynamic behaviour of the Sun is driven by the magnetic field since, in the outer atmosphere, it represents the largest source of energy by far. The interior of the Sun possesses a strong shear layer at the base of the convection zone, where sunspot magnetic fields are generated. A small-scale dynamo may also be operating near the surface of the Sun, generating magnetic fields that thread the lowest layer of the solar atmosphere, the turbulent photosphere. Above the photosphere lies the highly dynamic fine-scale chromosphere, and beyond that is the rare corona at high temperatures exceeding 1 million degrees K. Possible magnetic mechanisms for heating the corona and driving the solar wind (two intriguing and unsolved puzzles) are described. Other puzzles include the structure of giant flux ropes, known as prominences, which have complex fine structure. Occasionally, they erupt and produce huge ejections of mass and magnetic fields (coronal mass ejections), which can disrupt the space environment of the Earth. When such eruptions originate in active regions around sunspots, they are also associated with solar flares, in which magnetic energy is converted to kinetic energy, heat and fast-particle energy. A new theory will be presented for the origin of the twist that is observed in erupting prominences and for the nature of reconnection in the rise phase of an eruptive flare or coronal mass ejection.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofAnnales Geophysicaeen
dc.rights© Author(s) 2017. Published by Copernicus Publications on behalf of the European Geosciences Union. This work is distributed under the Creative Commons Attribution 3.0 License.en
dc.subjectSolar physics astrophysics astronomy (corona and transition region)en
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectGeologyen
dc.subjectAtmospheric Scienceen
dc.subjectEarth and Planetary Sciences (miscellaneous)en
dc.subjectSpace and Planetary Scienceen
dc.subject.lccQBen
dc.titleOur dynamic sun : 2017 Hannes Alfvén Medal lecture at the EGUen
dc.typeJournal itemen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.5194/angeo-35-805-2017
dc.description.statusPeer revieweden


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