We are pleased to announce that the winner of the ESPD Media of the Month contest for April is Daniel Nóbrega-Siverio (University of Oslo), with the following image of a coronal jet and surge in a radiation-MHD numerical simulation:

Description: This figure shows a snapshot from a solar bidimensional radiation-magnetohydrodynamic (R-MHD) numerical experiment by Nóbrega-Siverio et al. (2017, 2018) carried out using the Bifrost code (Gudiksen et al. 2011). In the left panel, a temperature, T, map from that simulation is shown, spanning from the upper layers of the convection zone up to the solar corona, where the location of the solar surface is indicated with a dash line at Z=0 Mm. In that panel, we can distinguish a dome-like structure that corresponds to a new emerged plasma that has raised from the solar interior and that is now being reconnected with the pre-existing coronal magnetic field. As a consequence of this magnetic reconnection process, two ejections are produced: a hot collimated coronal jet with an inverted-Y shape (or Eiffel tower) that reaches more than 1 MK; and a non-collimated ejection with a fang shape, known as surge, composed by cool plasma. The middle panel contains a map of the vertical velocity, uz, for the same instant and domain illustrated in the left panel. This panel shows that the coronal jet reaches velocities of more 150 km/s, in fact, the upwards velocities are up to 300 km/s (the color scale is saturated), while the surge has downward velocities, as maximum, of -50 km/s. The right panel contains a zoom out for the previous panel to highlight the reconnection site and the bidirectionial flow that leads to the hot coronal jet.

See full resolution image on Wikimedia Commons.