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dc.contributor.authorAntolin, P
dc.date.accessioned2019-12-20T15:30:05Z
dc.date.available2019-12-20T15:30:05Z
dc.date.issued2019-11-20
dc.identifier.citationAntolin , P 2019 , ' Thermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsations ' , Plasma Physics and Controlled Fusion , vol. 62 , no. 1 , 014016 . https://doi.org/10.1088/1361-6587/ab5406en
dc.identifier.issn0741-3335
dc.identifier.otherPURE: 264666365
dc.identifier.otherPURE UUID: 642d9967-3d9f-4462-b9e6-98398a8572c0
dc.identifier.otherBibtex: Antolin_2019
dc.identifier.otherScopus: 85076418740
dc.identifier.otherWOS: 000500001000001
dc.identifier.urihttps://hdl.handle.net/10023/19182
dc.descriptionPA acknowledges funding from his STFC Ernest Rutherford Fellowship (No. ST/R004285/1) and support from the International Space Science Institute, Bern, Switzerland to the International Teams on 'Implications for coronal heating and magnetic fields from coronal rain observations and modeling' (PI: P Antolin) and 'Observed Multi-Scale Variability of Coronal Loops as a Probe of Coronal Heating' (PIs: C Froment and P Antolin).en
dc.description.abstractThe complex interaction of the magnetic field with matter is the key to some of the most puzzling observed phenomena at multiple scales across the Universe, from tokamak plasma confinement experiments in the laboratory to the filamentary structure of the interstellar medium. A major astrophysical puzzle is the phenomenon of coronal heating, upon which the most external layer of the solar atmosphere, the corona, is sustained at multi-million degree temperatures on average. However, the corona also conceals a cooling problem. Indeed, recent observations indicate that, even more mysteriously, like snowflakes in the oven, the corona hosts large amounts of cool material termed coronal rain, hundreds of times colder and denser, that constitute the seed of the famous prominences. Numerical simulations have shown that this cold material does not stem from the inefficiency of coronal heating mechanisms, but results from the specific spatio-temporal properties of these. As such, a large fraction of coronal loops, the basic constituents of the solar corona, are suspected to be in a state of thermal non-equilibrium (TNE), characterised by heating (evaporation) and cooling (condensation) cycles whose telltale observational signatures are long-period intensity pulsations in hot lines and thermal instability-driven coronal rain in cool lines, both now ubiquitously observed. In this paper, we review this yet largely unexplored strong connection between the observed properties of hot and cool material in TNE and instability and the underlying coronal heating mechanisms. Focus is set on the long-observed coronal rain, for which significant research already exists, contrary to the recently discovered long-period intensity pulsations. We further identify the outstanding open questions in what constitutes a new, rapidly growing field of solar physics.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofPlasma Physics and Controlled Fusionen
dc.rightsCopyright © 2019 IOP Publishing Ltd. Open Access article. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en
dc.subjectSolar coronaen
dc.subjectSolar prominencesen
dc.subjectCoronal rainen
dc.subjectThermal instabilityen
dc.subjectThermal non-equilibriumen
dc.subjectMagnetohydrodynamicsen
dc.subjectMHD wavesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsationsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1088/1361-6587/ab5406
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/R004285/1en


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