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EP: Fachverband Extraterrestrische Physik
EP 6: Sun and Heliosphere III
EP 6.5: Talk
Tuesday, April 1, 2025, 17:30–17:45, ZHG101
A blowout jet in a self-consistent model of a solar coronal hole region — •Yajie Chen1, Hardi Peter1, 2, Damien Przybylski1, Lakshmi Pradeep Chitta1, and Sudip Mandal1 — 1Max-Planck Institute for Solar System Research, 37077 Goettingen, Germany — 2Institut für Sonnenphysik (KIS), 79110 Freiburg, Germany
Solar blowout jets are a distinct subclass of ubiquitous EUV and X-ray coronal jets. Most existing numerical models of blowout jets rely on prescribed initial magnetic field configurations or manual modifications of the magnetic field in the photosphere to trigger the jets. In this study, we first construct a comprehensive self-consistent 3D radiation MHD model of a solar coronal hole region, extending from the upper convection zone to the lower corona. Subsequently, we synthesize emissions in several EUV and X-ray passbands and identify a blowout jet self-consistently created in the model. The jet initially appears as a standard jet but later evolves into a blowout jet. The jet has a width of ~10 Mm and a lifetime of ~10 minutes. The plasma speeds within the jet reach approximately 180 km/s, and we also find a faint component in the synthesized X-ray images propagating at Alfvén speeds of ~500 km/s, which can be attributed to heating fronts. The corresponding magnetograms in the modeled photosphere show signatures of flux emergence and cancellation. These characteristics match well with those observed in blowout jets. By examining the magnetic field lines in and around the jet base, we validate the scenario that the jet is triggered by magnetic reconnection between the newly emerged twisted closed loops and the pre-existing open field lines.
Keywords: Sun: magnetic fields; Sun: corona; Magnetohydrodynamics (MHD)