  In this Letter, we investigate the long-duration quasi-static evolution of 12
pre-eruptive filaments (4 active region and 8 quiescent filaments), mainly
focusing on the evolution of the filament height in three dimension (3D) and
the decay index of the background magnetic field. The filament height in 3D is
derived through two-perspective observations of \textit{Solar Dynamics
Observatory} and \textit{Solar TErrestrial RElations Observatory}. The coronal
magnetic field is reconstructed using the potential field source surface model.
A new finding is that the filaments we studied show two types of long-duration
evolution: one type is comprised of a long-duration static phase and a short
slow rise phase with a duration of less than 12 hours and a speed of 0.1--0.7
km s$^{-1}$, while the other one only presents a slow rise phase but with an
extremely long duration of more than 60 hours and a smaller speed of 0.01--0.2
km s$^{-1}$. At the moment approaching the eruption, the decay index of the
background magnetic field at the filament height is similar for both active
region and quiescent filaments. The average value and upper limit are $\sim$0.9
and $\sim$1.4, close to the critical index of torus instability. Moreover, the
filament height and background magnetic field strength are also found to be
linearly and exponentially related with the filament length, respectively.
