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dc.contributor.authorChen, Huadong
dc.contributor.authorZhang, Jun
dc.contributor.authorDe Pontieu, Bart
dc.contributor.authorMa, Suli
dc.contributor.authorKliem, Bernhard
dc.contributor.authorPriest, Eric
dc.date.accessioned2020-09-08T08:30:03Z
dc.date.available2020-09-08T08:30:03Z
dc.date.issued2020-08-10
dc.identifier.citationChen , H , Zhang , J , De Pontieu , B , Ma , S , Kliem , B & Priest , E 2020 , ' Coronal mini-jets in an activated solar tornado-like prominence ' , Astrophysical Journal , vol. 899 , no. 1 , 19 . https://doi.org/10.3847/1538-4357/ab9caden
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 269926308
dc.identifier.otherPURE UUID: 7fc62f24-ef4d-446c-915f-3cf7e6fee0a7
dc.identifier.otherScopus: 85089594257
dc.identifier.otherORCID: /0000-0003-3621-6690/work/79917741
dc.identifier.otherWOS: 000560897000001
dc.identifier.urihttps://hdl.handle.net/10023/20580
dc.description.abstractHigh-resolution observations from the Interface Region Imaging Spectrometer reveal the existence of a particular type of small solar jet, which arose singly or in clusters from a tornado-like prominence suspended in the corona. In this study, we perform a detailed statistical analysis of 43 selected mini-jets in the tornado event. Our results show that the mini-jets typically have (1) a projected length of 1.0–6.0 Mm, (2) a width of 0.2–1.0 Mm, (3) a lifetime of 10–50 s, (4) a velocity of 100–350 km s−1, and (5) an acceleration of 3–20 km s−2. Based on spectral diagnostics and EM-Loci analysis, these jets seem to be multithermal small-scale plasma ejections with an estimated average electron density of ~2.4  ×  1010 cm−3 and an approximate mean temperature of ~2.6  ×  105 K. Their mean kinetic energy density, thermal energy density, and dissipated magnetic field strength are roughly estimated to be ~9 erg cm−3, 3 erg cm−3, and 16 G, respectively. The accelerations of the mini-jets, the UV and EUV brightenings at the footpoints of some mini-jets, and the activation of the host prominence suggest that the tornado mini-jets are probably created by fine-scale external or internal magnetic reconnections (a) between the prominence field and the enveloping or background field or (b) between twisted or braided flux tubes within the prominence. The observations provide insight into the geometry of such reconnection events in the corona and have implications for the structure of the prominence magnetic field and the instability that is responsible for the eruption of prominences and coronal mass ejections.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2020. The Author(s). Published by the American Astronomical Society. Open Access article. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en
dc.subjectThe Sunen
dc.subjectSolar activityen
dc.subjectSolar prominencesen
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectDASen
dc.subject.lccQBen
dc.titleCoronal mini-jets in an activated solar tornado-like prominenceen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ab9cad
dc.description.statusPeer revieweden


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