  The morphology of molecular clouds is crucial for understanding their origin
and evolution. In this work, we investigate the morphology of the filamentary
molecular clouds (filaments for short) using a portion of the $^{12}\text{CO}
(J=1-0)$ data from the Milky Way Imaging Scroll Painting (MWISP) project. The
data cover an area spanning $104.75^\circ <l< 150.25^\circ , \vert b\vert <
5.25^\circ$ in Galactic coordinates, with $V_\text{LSR}$ ranging from $-95$ to
25 $\text{km s}^{-1}$. Our primary focus is on the orientation and
morphological asymmetry of the filaments. To achieve this, we apply several
criteria on the data to create a sample of filaments with well-defined straight
shape, and we use elliptical fitting to obtain the orientation of each
filament, with an estimated error of $\sim1.6^\circ$ for the orientation. We
find that the filament orientation with respect to the Galactic plane exhibits
a bimodal distribution, a double-Gaussian fitting of which has two centres
located at $-38.1^\circ $ and $42.0^\circ $, with 1$\sigma$ of the two Gaussian
functions being $35.4^\circ$ and $27.4^\circ$. We do not find significant
correlation between the orientation and other parameters, including the
Galactic coordinates, radial velocity, velocity width, and physical scale. A
considerable fraction of filaments ($\gtrsim 40$ per cent) display head-tail
asymmetry, which suggests that mass concentration tends to occur at one end of
the filaments.
