  It is generally believed that filament formation involves a process of the
accumulation of magnetic energy. However, in this paper we discuss the idea
that filaments will not erupt and will only deform when the stored magnetic
energy is released gradually. Combining high-quality observations from Solar
Dynamics Observatory and other instruments, we present the formation and
immediate deformation of a small filament (F1) in the active region (AR) 12760
on 28-30 April 2020. Before the filament formation, three successive dipoles
quickly emerged with separation motions in the center of AR 12760. Due to the
magnetic interaction between magnetic dipoles and pre-existing positive
polarities, coronal brightenings consequently appeared in the overlying
atmosphere. Subsequently, because of the continuous cancellation of magnetic
flux that happened around the adjacent ends of F1 and another nearby filament
(F2), the magnetic reconections occurred intermittently occurred between F1 and
F2. Finally, F1 lessened in the shear, and F2 became shorter. All the results
show that the formation of F1 was closely associated with intermittent
interactions between the sequence of emerging dipoles and pre-existing magnetic
polarities, and the immediate deformation of F1 was intimately related to
intermittent interactions between F1 and F2. We also suggest that the
intermittent magnetic interactions driven by the continuous magnetic activities
(magnetic-flux emergence, cancellation, and convergence) play an important role
in the formation and deformation of filaments.
