A self-consistent 3D magnetohydrodynamic model producing a solar blowout jet

Context. Solar blowout jets are a distinct subclass of ubiquitous extreme-ultraviolet (EUV) and X-ray coronal jets. Aims. Most existing models of blowout jets prescribe initial magnetic-field configurations and apply ad hoc changes in the photosphere to trigger the jets. In contrast, we aim for a self-consistent magneto-convective description of the jet initiation. Methods. We employed a 3D radiation magnetohydrodynamic (MHD) model of a solar coronal hole region using the MURaM code. The computational domain extends from the upper convection zone to the lower corona. We synthesized the emission in the EUV and X-ray for direct comparison with observations and examined the evolution of the magnetic-field structure of the event. Results. In the simulation a twisted flux tube forms self-consistently, emerges through the surface, and interacts with the preexisting open field. Initially, the resulting jet is of the standard type with a narrow spire. The release of the twist into the open field causes a broadening of the jet spire, turning the jet into a blowout type. At the same time, this creates a fast heating front, propagating at the local Alfvén speed. The properties of the modeled jet closely match those of the observed blowout jets: a slow (∼180 km s−1) mass upflow and a fast (∼500 km s−1) propagating front form, the latter being a signature of the heating front. Also, the timing of the jet with respect to flux emergence and subsequent cancellation matches observations. Conclusions. Near-surface magneto-convection self-consistently generates a twisted flux tube that emerges through the photosphere. The tube then interacts with the preexisting magnetic field by means of interchange reconnection. This transfers the twist to the open field and produces a blowout jet that matches the main characteristics of that found in observations.