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dc.contributor.authorSyntelis, P.
dc.contributor.authorArchontis, V.
dc.contributor.authorTsinganos, K.
dc.date.accessioned2019-05-24T15:35:15Z
dc.date.available2019-05-24T15:35:15Z
dc.date.issued2019-05-03
dc.identifier.citationSyntelis , P , Archontis , V & Tsinganos , K 2019 , ' Recurrent CME-like eruptions in emerging flux regions. II. Scaling of energy and collision of successive eruptions ' , Astrophysical Journal , vol. 876 , no. 1 , 61 . https://doi.org/10.3847/1538-4357/ab16d2en
dc.identifier.issn1538-4357
dc.identifier.otherPURE: 259078780
dc.identifier.otherPURE UUID: 40beea0d-b50d-45f3-be00-ca9b881df2a6
dc.identifier.otherRIS: urn:10DE9EB3D5ABD38A56C728FB538741A9
dc.identifier.otherScopus: 85067303134
dc.identifier.otherWOS: 000466892200008
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700876
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131788
dc.identifier.urihttp://hdl.handle.net/10023/17758
dc.descriptionThis project has received funding from the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1. The authors acknowledge support by the Royal Society. This work was supported by computational time granted from the Greek Research & Technology Network (GRNET) in the National HPC facility—ARIS.en
dc.description.abstractWe present results of three-dimensional MHD simulations of recurrent eruptions in emerging flux regions. The initial numerical setup is the same as that in the work by Syntelis et al. Here, we perform a parametric study on the magnetic field strength (B 0) of the emerging field. The kinetic energy of the produced ejective eruptions in the emerging flux region ranges from 1026 to 1028 erg, reaching up to the energies of small coronal mass ejections. The kinetic and magnetic energies of the eruptions scale linearly in a logarithmic plot. We find that the eruptions are triggered earlier for higher B 0 and that B 0 is not directly correlated to the frequency of occurrence of the eruptions. Using large numerical domains, we show the initial stage of the partial merging of two colliding erupting fields. The partial merging occurs partly by the reconnection between the field lines of the following and the leading eruption at the interface between them. We also find that tether-cutting reconnection of the field lines of the leading eruption underneath the following eruption magnetically links the two eruptions. Shocks develop inside the leading eruption during the collision.
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2019. 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/ab16d2en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectSun: activityen
dc.subjectSun: interioren
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectNDASen
dc.subject.lccQBen
dc.titleRecurrent CME-like eruptions in emerging flux regions. II. Scaling of energy and collision of successive 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/ab16d2
dc.description.statusPeer revieweden


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