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dc.contributor.authorTerradas, J.
dc.contributor.authorSoler, R.
dc.contributor.authorLuna, M.
dc.contributor.authorOliver, R.
dc.contributor.authorBallester, J. L.
dc.contributor.authorWright, Andrew Nicholas
dc.date.accessioned2016-04-29T10:30:03Z
dc.date.available2016-04-29T10:30:03Z
dc.date.issued2016-03-30
dc.identifier.citationTerradas , J , Soler , R , Luna , M , Oliver , R , Ballester , J L & Wright , A N 2016 , ' Solar prominences embedded in flux ropes : morphological features and dynamics from 3D MHD simulations ' Astrophysical Journal , vol. 820 , no. 2 , pp. 1-14 . DOI: 10.3847/0004-637X/820/2/125en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 241556677
dc.identifier.otherPURE UUID: c017875c-f923-47c2-ac3d-f69c58377647
dc.identifier.otherScopus: 84962860779
dc.identifier.urihttp://hdl.handle.net/10023/8702
dc.descriptionJ.T. and R.S. acknowledge support from MINECO and UIB through a Ramón y Cajal grant. The authors acknowledge support by the Spanish MINECO and FEDER funds through project AYA2014-54485-P. M.L. acknowledges the support by the Spanish Ministry of Economy and Competitiveness through projects AYA2011-24808, AYA2010-18029, and AYA2014-55078-P. This work contributes to the deliverables identified in FP7 European Research Council grant agreement 277829, “Magnetic Connectivity through the Solar Partially Ionized Atmosphere” (PI: E. Khomenko). M.L., J.T., and J.L.B. also acknowledge support from the International Space Science Institute (ISSI) to the Team 314 on “Large-Amplitude Oscillation in prominences” led by M. Luna.en
dc.description.abstractThe temporal evolution of a solar prominence inserted in a three-dimensional magnetic flux rope is investigated numerically. Using the model of Titov & Démoulin (1999) under the regime of weak twist, the cold and dense prominence counteracts gravity by modifying the initially force-free magnetic configuration. In some cases a quasi-stationary situation is achieved after the relaxation phase, characterized by the excitation of standing vertical oscillations. These oscillations show a strong attenuation with time produced by the mechanism of continuum damping due to the in homogeneous transition between the prominence and solar corona. The characteristic period of the vertical oscillations does not depend strongly on the twist of the flux rope. Nonlinearity is the responsible for triggering the Kelvin-Helmholtz instability associated to the vertical oscillations and that eventually produces horizontal structures. Contrary to other configurations in which the longitudinal axis of the prominence is permeated by a perpendicular magnetic field, like in unsheared arcades, the orientation of the prominence along the flux rope axis prevents the development of Rayleigh-Taylor instabilities and therefore the appearance of vertical structuring along this axis.en
dc.format.extent14en
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016 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/10.3847/0004-637X/820/2/125en
dc.subjectMagnetic fieldsen
dc.subjectPlasmasen
dc.subjectSun: coronaen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSolar prominences embedded in flux ropes : morphological features and dynamics from 3D MHD simulationsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/820/2/125
dc.description.statusPeer revieweden


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