  Prominences, or filaments, are a striking phenomenon in the solar atmosphere.
Besides their own rich features and dynamics, they are related to many other
activities, such as solar flares and coronal mass ejections (CMEs). In the past
several years we have been investigating the prominence formation,
oscillations, and eruptions through both data analysis and radiative
hydrodynamic and magnetohydrodynamic (MHD) simulations. This paper reviews our
progress on these topics, which includes: (1) With updated radiative cooling
function, the coronal condensation becomes a little faster than previous work;
(2) Once a seed condensation is formed, it can grow via siphon flow
spontaneously even if the evaporation stops; (3) A scaling law was obtained to
relate the length of the prominence thread to various parameters, indicating
that higher prominences tend to have shorter threads, which is consistent with
the fact that threads are long in active region prominences and short in
quiescent prominences; (4) It was proposed that long-time prominence
oscillations out of phase might serve as a precursor for prominence eruptions
and CMEs; (5) An ensemble of oscillating prominence threads may explain the
counter-streaming motion.
