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dc.contributor.authorChen, Jie
dc.contributor.authorSu, Jiangtao
dc.contributor.authorDeng, Yuanyong
dc.contributor.authorPriest, E. R.
dc.date.accessioned2017-06-01T13:30:11Z
dc.date.available2017-06-01T13:30:11Z
dc.date.issued2017-05-04
dc.identifier.citationChen , J , Su , J , Deng , Y & Priest , E R 2017 , ' A complex solar coronal jet with two phases ' Astrophysical Journal , vol. 840 , no. 1 , 54 . https://doi.org/10.3847/1538-4357/aa6c59en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 250153321
dc.identifier.otherPURE UUID: 4ef85ce9-ce24-4990-b5c1-b9bc218c2534
dc.identifier.otherScopus: 85019159292
dc.identifier.urihttp://hdl.handle.net/10023/10893
dc.descriptionThis work was partly supported by National Natural Science Foundation of China (grant Nos. 11303048, 11673033, 11373040, 11427901). This work was also partly supported by an International Exchanges cost share award with NSFC for overseas travel between collaborators in the UK and China, and State Key Laboratory for Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences.en
dc.description.abstractJets often occur repeatedly from almost the same location. In this paper, a complex solar jet was observed with two phases to the west of NOAA AR 11513 on 2012 July 2. If it had been observed at only moderate resolution, the two phases and their points of origin would have been regarded as identical. However, at high resolution we find that the two phases merge into one another and the accompanying footpoint brightenings occur at different locations. The phases originate from different magnetic patches rather than being one phase originating from the same patch. Photospheric line of sight (LOS) magnetograms show that the bases of the two phases lie in two different patches of magnetic flux that decrease in size during the occurrence of the two phases. Based on these observations, we suggest that the driving mechanism of the two successive phases is magnetic cancellation of two separate magnetic fragments with an opposite-polarity fragment between them.en
dc.format.extent8en
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/aa6c59en
dc.subjectMagnetic reconnectionen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: activityen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectNDASen
dc.subject.lccQBen
dc.titleA complex solar coronal jet with two phasesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa6c59
dc.description.statusPeer revieweden


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