Evolution and dynamics of a solar active prominence

The life of a solar active prominence, one of the most remarkable objects on the Sun, is full of dynamics; after first appearing on the Sun, the prominence continuously evolves with various internal motions and eventually produces a global eruption toward interplanetary space. Here we report that the whole life of an active prominence is successfully reproduced by performing as long-term a magnetohydrodynamic simulation of a magnetized prominence plasma as was ever done. The simulation reveals underlying dynamic processes that give rise to observed properties of an active prominence: invisible subsurface flows self-consistently produce the cancellation of magnetic flux observed in the photosphere, while observed but somewhat counterintuitive strong upflows are driven against gravity by enhanced gas pressure gradient force along a magnetic field line locally standing vertical. The most highlighted dynamic event, transition into an eruptive phase, occurs as a natural consequence of the self-consistent evolution of a prominence plasma interacting with a magnetic field, which is obtained by seamlessly reproducing dynamic processes involved in the formation and eruption of an active prominence.