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dc.contributor.authorAntolin, P.
dc.contributor.authorVissers, G.
dc.contributor.authorPereira, T. M. D.
dc.contributor.authorRouppe van der Voort, L.
dc.contributor.authorScullion, E.
dc.date.accessioned2017-02-14T11:30:11Z
dc.date.available2017-02-14T11:30:11Z
dc.date.issued2015-06-09
dc.identifier248969440
dc.identifier8f764c31-f9aa-4340-8935-5a2cf2cf0506
dc.identifier84934960659
dc.identifier.citationAntolin , P , Vissers , G , Pereira , T M D , Rouppe van der Voort , L & Scullion , E 2015 , ' The multi-thermal and multi-stranded nature of coronal rain ' , Astrophysical Journal , vol. 806 , 81 . https://doi.org/10.1088/0004-637X/806/1/81en
dc.identifier.issn0004-637X
dc.identifier.otherBibCode: 2015ApJ...806...81A
dc.identifier.urihttps://hdl.handle.net/10023/10290
dc.description.abstractWe analyze coordinated observations of coronal rain in loops, spanning chromospheric, transition region (TR), and coronal temperatures with sub-arcsecond spatial resolution. Coronal rain is found to be a highly multithermal phenomenon with a high degree of co-spatiality in the multi-wavelength emission. EUV darkening and quasi-periodic intensity variations are found to be strongly correlated with coronal rain showers. Progressive cooling of coronal rain is observed, leading to a height dependence of the emission. A fast-slow two-step catastrophic cooling progression is found, which may reflect the transition to optically thick plasma states. The intermittent and clumpy appearance of coronal rain at coronal heights becomes more continuous and persistent at chromospheric heights just before impact, mainly due to a funnel effect from the observed expansion of the magnetic field. Strong density inhomogeneities of 0.″2-0.″5 are found, in which a transition from temperatures of 105 to 104 K occurs. The 0.″2-0.″8 width of the distribution of coronal rain is found to be independent of temperature. The sharp increase in the number of clumps at the coolest temperatures, especially at higher resolution, suggests that the bulk distribution of the rain remains undetected. Rain clumps appear organized in strands in both chromospheric and TR temperatures. We further find structure reminiscent of the magnetohydrodynamic (MHD) thermal mode (also known as entropy mode), thereby suggesting an important role of thermal instability in shaping the basic loop substructure. Rain core densities are estimated to vary between 2 × 1010 and 2.5 × 1011cm−3, leading to significant downward mass fluxes per loop of 1–5 × 109 g s−1, thus suggesting a major role in the chromosphere-corona mass cycle.
dc.format.extent21
dc.format.extent2757396
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectInstabilitiesen
dc.subjectMagnetohydrodynamics: MHDen
dc.subjectSun: activityen
dc.subjectSun: coronaen
dc.subjectSun: filamentsen
dc.subjectProminencesen
dc.subjectWavesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe multi-thermal and multi-stranded nature of coronal rainen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doi10.1088/0004-637X/806/1/81
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015ApJ...806...81Aen


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