Flux emergence of a non twisted magnetic flux tube

We study the numerical simulation of a weakly twisted magnetic flux tube emergence in a non magnetized corona. We find that this flux tube creates a system of two expanding magnetic lobes, that exist over the photospheric bipolar magnetic region and are separated by the polarity inversion line. Those structures expand due to the magnetic pressure, creating a current sheet that leads to the reconnection of the magnetic field lines. This continuous interaction ejects chromospheric plasma to the upper atmosphere and heats plasma up to 2MK, creating a sequence of cool and hot coronal jets. Due to the reconnection, the initial emerging field creates hot and cool loops in the active region, and leads to the formation of a confined twisted flux rope inside the magnetic envelope. We created synthetic AIA and XRT images of the simulation to see whether those structures could be observed. We find that only some of the ejection can be identified in the synthetic images, and that some cool and dense structures could be misinterpreted as very warm in high temperature filters.