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dc.contributor.authorSyntelis, P.
dc.contributor.authorArchontis, V.
dc.contributor.authorTsinganos, K.
dc.date.accessioned2018-08-15T14:30:08Z
dc.date.available2018-08-15T14:30:08Z
dc.date.issued2017-11-21
dc.identifier.citationSyntelis , P , Archontis , V & Tsinganos , K 2017 , ' Recurrent CME-like eruptions in emerging flux regions. I. On the mechanism of eruptions ' , Astrophysical Journal , vol. 850 , no. 1 , 95 . https://doi.org/10.3847/1538-4357/aa9612en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 255392308
dc.identifier.otherPURE UUID: 65ed2e0d-611c-4874-8d6d-8ced2e75acf8
dc.identifier.otherBibCode: 2017ApJ...850...95S
dc.identifier.otherScopus: 85037686964
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700855
dc.identifier.otherWOS: 000415950200007
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131782
dc.identifier.urihttp://hdl.handle.net/10023/15825
dc.descriptionThis project has received funding from the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1. This research has been co-financed by the European Union (European Social Fund—ESF) and Greek national funds through the Operational Program “Education and Lifelong Learning” of the National Strategic Reference Framework (NSRF)—Research Funding Program: Thales Investing in Knowledge Society through the European Social Fund. The authors acknowledge support by the Royal Society.en
dc.description.abstractWe report on three-dimensional (3D) magnetohydrodynamic (MHD) simulations of recurrent eruptions in emerging flux regions. We find that reconnection of sheared field lines, along the polarity inversion line of an emerging bipolar region, leads to the formation of a new magnetic structure, which adopts the shape of a magnetic flux rope (FR) during its rising motion. Initially, the FR undergoes a slow-rise phase and, eventually, it experiences a fast-rise phase and ejective eruption toward the outer solar atmosphere. In total, four eruptions occur during the evolution of the system. For the first eruption, our analysis indicates that the torus instability initiates the eruption and that tether-cutting reconnection of the field lines, which envelop the FR, triggers the rapid acceleration of the eruptive field. For the following eruptions, we conjecture that it is the interplay between tether-cutting reconnection and torus instability that causes the onset of the various phases. We show the 3D shape of the erupting fields, focusing more on how magnetic field lines reconnect during the eruptions. We find that when the envelope field lines reconnect mainly with themselves, hot and dense plasma is transferred closer to the core of the erupting FR. The same area appears to be cooler and less dense when the envelope field lines reconnect with neighboring sheared field lines. The plasma density and temperature distribution, together with the rising speeds, energies, and size of the erupting fields, indicate that they may account for small-scale (mini) coronal mass ejections.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017 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://doi.org/10.3847/1538-4357/aa9612en
dc.subjectMagnetohydrodynamics: MHDen
dc.subjectMethods: numericalen
dc.subjectSun: activityen
dc.subjectSun: interioren
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleRecurrent CME-like eruptions in emerging flux regions. I. On the mechanism of eruptionsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa9612
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1711.10249en


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