  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 the interplane- tary space. Here we report that the
whole life of an active prominence is successfully re- produced 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 at the
photosphere, while observed and somewhat counterintuitive strong upflows are
driven against gravity by en- hanced 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 con- sequence 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 forma- tion and eruption of an active prominence.
