  The interiors of quiescent prominences are filled with turbulent flows. The
evolution of upflow plumes, descending pillars, and vortex motions has been
clearly detected in high-resolution observations. The Rayleigh-Taylor
instability is thought to be a driver of such internal flows. Descending
pillars are related to the mass budgets of prominences. There is a hypothesis
of dynamic equilibrium where the mass drainage via descending pillars and the
mass supply via radiative condensation are balanced to maintain the prominence
mass; however, the background physics connecting the two different processes is
poorly understood. In this study, we reproduced the dynamic interior of a
prominence via radiative condensation and the mechanism similar to the
Rayleigh-Taylor instability using a three-dimensional magnetohydrodynamic
simulation including optically thin radiative cooling and nonlinear anisotropic
thermal conduction. The process to prominence formation in the simulation
follows the reconnection-condensation model, where topological change in the
magnetic field caused by reconnection leads to radiative condensation.
Reconnection is driven by converging motion at the footpoints of the coronal
arcade fields. In contrast to the previous model, by randomly changing the
speed of the footpoint motion along a polarity inversion line, the dynamic
interior of prominence is successfully reproduced. We find that the mass
condensation rate of the prominence is enhanced in the case with dynamic state.
Our results support the observational hypothesis that the condensation rate is
balanced with the mass drainage rate and suggest that a self-induced mass
maintenance mechanism exists.
