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dc.contributor.authorScullion, E.
dc.contributor.authorRouppe van der Voort, L.
dc.contributor.authorWedemeyer, S.
dc.contributor.authorAntolin, P.
dc.date.accessioned2017-02-14T10:30:23Z
dc.date.available2017-02-14T10:30:23Z
dc.date.issued2014-11-24
dc.identifier.citationScullion , E , Rouppe van der Voort , L , Wedemeyer , S & Antolin , P 2014 , ' Unresolved fine-scale structure in solar coronal loop-tops ' , Astrophysical Journal , vol. 797 , 36 . https://doi.org/10.1088/0004-637X/797/1/36en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 248969759
dc.identifier.otherPURE UUID: b44dda17-2073-4f33-a574-61f07db5acc2
dc.identifier.otherBibCode: 2014ApJ...797...36S
dc.identifier.otherScopus: 84914678265
dc.identifier.urihttp://hdl.handle.net/10023/10288
dc.description.abstractNew and advanced space-based observing facilities continue to lower the resolution limit and detect solar coronal loops in greater detail. We continue to discover even finer substructures within coronal loop cross-sections, in order to understand the nature of the solar corona. Here, we push this lower limit further to search for the finest coronal loop substructures, through taking advantage of the resolving power of the Swedish 1 m Solar Telescope/CRisp Imaging Spectro-Polarimeter (CRISP), together with co-observations from the Solar Dynamics Observatory/Atmospheric Image Assembly (AIA). High-resolution imaging of the chromospheric Hα 656.28 nm spectral line core and wings can, under certain circumstances, allow one to deduce the topology of the local magnetic environment of the solar atmosphere where its observed. Here, we study post-flare coronal loops, which become filled with evaporated chromosphere that rapidly condenses into chromospheric clumps of plasma (detectable in Hα) known as a coronal rain, to investigate their fine-scale structure. We identify, through analysis of three data sets, large-scale catastrophic cooling in coronal loop-tops and the existence of multi-thermal, multi-stranded substructures. Many cool strands even extend fully intact from loop-top to footpoint. We discover that coronal loop fine-scale strands can appear bunched with as many as eight parallel strands within an AIA coronal loop cross-section. The strand number density versus cross-sectional width distribution, as detected by CRISP within AIA-defined coronal loops, most likely peaks at well below 100 km, and currently, 69% of the substructure strands are statistically unresolved in AIA coronal loops.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1088/0004-637X/797/1/36en
dc.subjectMethods: data analysisen
dc.subjectMethods: observationalen
dc.subjectTechniques: image processingen
dc.subjectTechniques: spectroscopicen
dc.subjectTelescopesen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleUnresolved fine-scale structure in solar coronal loop-topsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/797/1/36
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2014ApJ...797...36Sen


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