  For the first time, based on long-term spectral monitoring with high spectral
resolution, the optical spectrum of the weak central star of the IR source
RAFGL 5081 has been studied. The spectral type of this star is close to G5-8
II, and its effective temperature is Teff ~5400 K. An unusual spectral
phenomenon was discovered: splitting of the profiles of broad, stationary
absorption lines of medium and low intensity. The heliocentric radial
velocities Vr of all components of metal absorption lines, the NaI D lines, and
the H$\alpha$ line were measured for all the observation epochs. The constancy
of the absorption lines rules out the possibility that the line splitting is
due to binarity. The radial velocities of the wind components in the profiles
of the NaI D and H$\alpha$ lines reach $-250$ and $-600$ km/s, respectively.
These profiles have narrow components, whose number, depth, and position vary
with time. The time variability and multicomponent structure of the profiles of
the NaI D and H$\alpha$ lines indicates inhomogeneity and instability of the
circumstellar envelope of RAFGL 5081. The presence of components with velocity
Vr(IS)=$-65$ km/s in the NaI(1) lines provides evidence that RAFGL 5081 is
located behind the Perseus arm, i.e., no closer than 2 kpc. It is noted that
RAFGL 5081 is associated with the reflection nebula GN 02.44.7.
