Non-linear force-free field modelling of solar coronal jets in theoretical configurations
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Coronal 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 in understanding the dynamic processes involved, but previous studies tend to consider only one mechanism (e.g. emergence or rotation) for the origin of the jet. In this study we model a series of idealised archetypal jet configurations and follow the evolution of the coronal magnetic field. This is a step towards understanding these idealised 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 build up of free energy, reminiscent of the progenitors of so-called blowout jets, whereas other, simpler configurations are more comparable to the standard jetmodel. The next stage is a comparison with observed coronal jet structures and their corresponding photospheric evolution.
Meyer , K A , Savcheva , A S , Mackay , D H & DeLuca , E E 2019 , ' Non-linear force-free field modelling of solar coronal jets in theoretical configurations ' , Astrophysical Journal .
© 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://iopscience.iop.org/journal/0004-637X
DescriptionFunding: KAM and DHM acknowledge the support of the Leverhulme Trust, the STFC and the Carnegie Trustfor the Universities of Scotland.
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