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dc.contributor.authorMeyer, Karen Alison
dc.contributor.authorSavcheva, Antonia S.
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorDeLuca, Ed E.
dc.date.accessioned2019-05-02T15:30:08Z
dc.date.available2019-05-02T15:30:08Z
dc.date.issued2019-07-25
dc.identifier.citationMeyer , K A , Savcheva , A S , Mackay , D H & DeLuca , E E 2019 , ' Nonlinear force-free field modeling of solar coronal jets in theoretical configurations ' , Astrophysical Journal , vol. 880 , no. 1 , 62 , pp. 1-13 . https://doi.org/10.3847/1538-4357/ab271aen
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 258834139
dc.identifier.otherPURE UUID: 7d912f11-2aaf-4adb-adec-78e688eb6f6f
dc.identifier.otherScopus: 85071943426
dc.identifier.otherScopus: 85071943426
dc.identifier.otherORCID: /0000-0001-6065-8531/work/65345298
dc.identifier.urihttp://hdl.handle.net/10023/17635
dc.descriptionK.A.M. and D.H.M. gratefully acknowledge the support of the Leverhulme Trust, the STFC and the Carnegie Trust for the Universities of Scotland. K.A.M., A.S.S., and E.E.D. thank ISSI (Bern) for their support of the team "Understanding Solar Jets and their Role in Atmospheric Structure and Dynamics." D.H.M. thanks the EU for their support under FP7.en
dc.description.abstractCoronal jets occur frequently on the Sun, and may contribute significantly to the solar wind. With the suite of instruments available now, we can observe these phenomena in greater detail than ever before. Modeling and simulations can assist further with understanding the dynamic processes involved, but previous studies tended to consider only one mechanism (e.g., emergence or rotation) for the origin of the jet. In this study we model a series of idealized archetypal jet configurations and follow the evolution of the coronal magnetic field. This is a step toward understanding these idealized situations before considering their observational counterparts. Several simple situations are set up for the evolution of the photospheric magnetic field: a single parasitic polarity rotating or moving in a circular path; as well as opposite polarity pairs involved in flyby (shearing), cancellation or emergence; all in the presence of a uniform, open background magnetic field. The coronal magnetic field is evolved in time using a magnetofrictional relaxation method. While magnetofriction cannot accurately reproduce the dynamics of an eruptive phase, the structure of the coronal magnetic field, as well as the buildup of electric currents and free magnetic energy are instructive. Certain configurations and motions produce a flux rope and allow the significant buildup of free energy, reminiscent of the progenitors of so-called blowout jets, whereas other, simpler configurations are more comparable to the standard jet model. The next stage is a comparison with observed coronal jet structures and their corresponding photospheric evolution.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2019, American Astronomical Society. This work has been made available online in accordance with the publisher's policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/ab271aen
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-4357/ab271aen
dc.subjectSun: activityen
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleNonlinear force-free field modeling of solar coronal jets in theoretical configurationsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ab271a
dc.description.statusPeer revieweden


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