Coronal Jets Simulated with the Alfvén Wave Solar Model

In this paper we carry out numerical modeling of coronal jets to understand their effects on the global corona and their contribution to the solar wind. We simulated jet models implemented within a well established three dimensional, two-temperature magneto-hydrodynamic (MHD) solar corona model that is built upon kinetic Alvén wave dissipation, producing realistic solar wind background. The jet was produced by positioning a local magnetic bipole under the solar surface and rotating the boundary plasma around the bipole’s magnetic axis. The moving plasma dragged the magnetic field lines along with it, which constructed a similar jet model as decribed by Pariat et al. (2009). Even if we did not attempt to model any specific event, we compared line of sight synthetic images to multiple jet observations at EUV and X-ray bands, and found very close match in terms of physical structure, dynamics and intensity. We also found that by the end of the three hours of simulation the large-scale solar corona was affected by the outward propagating torsional Alfvén waves generated by the polar jet over 40 degrees in latitude and out to 24 solar radii. However, we estimated that polar jets contribute to the solar wind energy maximum only a few percent based on our idealized case. Subject headings: methods: numerical — MHD — Solar wind — Sun: corona — Sun: waves