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 amagnetohydrodynamic 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.
