  Highly-resolution optical spectra of the optical component of the IR-source
IRAS01005+7910 are used to determine the spectral type of its central star,
B1.5$ \pm $0.3, identify the spectral features, and analyze their profile and
radial velocity variations. The systemic velocity Vsys =$-50.5$ km/s is
determined from the positions of the symmetric and stable profiles of the
forbidden [NI], [NII], [OI], [SII], and [FeII] emission lines. The presence of
the [NII] and [SII] forbidden emissions indicates the onset of the ionization
of the circumstellar envelope and the fact that the star is very close to
undergoing the planetary nebula stage. The broad range of heliocentric radial
velocity Vr estimates based on the core lines, which amounts to about 34 km/s,
is partly due to the deformations of the profiles caused by variable emissions.
The variations of the Vr in the line wings are smaller, about 23 km/s, and may
be due to pulsations and/or hidden binarity of the star. The deformations of
the profiles of complex absorption-emission lines may result from variations of
their absorption components caused by the variations of the geometry and
kinematics in the wind base. The H$\alpha$ lines exhibit P Cyg III type wind
profiles. Deviations of the wind from spherical symmetry are shown to be small.
The relatively low wind velocity (27$\div$74 km/s from different observations)
and the strong intensity of the red emission (it exceeds the continuum level by
up to a factor of seven) are typical for hypergiants rather than the classical
supergiants. IRAS01005 +7910 is an example of spectral mimicry of a low mass
post-AGB star masquerading as a massive hypergiant.
