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Highly-resolution optical spectra of the optical component of the IR-sourceIRAS01005+7910 are used to determine the spectral type of its central star,B1.5$ \pm $0.3, identify the spectral features, and analyze their profile andradial velocity variations. The systemic velocity Vsys =$-50.5$ km/s isdetermined from the positions of the symmetric and stable profiles of theforbidden [NI], [NII], [OI], [SII], and [FeII] emission lines. The presence ofthe [NII] and [SII] forbidden emissions indicates the onset of the ionizationof the circumstellar envelope and the fact that the star is very close toundergoing the planetary nebula stage. The broad range of heliocentric radialvelocity 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 maybe due to pulsations and/or hidden binarity of the star. The deformations ofthe profiles of complex absorption-emission lines may result from variations oftheir absorption components caused by the variations of the geometry andkinematics in the wind base. The H$\alpha$ lines exhibit P Cyg III type windprofiles. 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 byup to a factor of seven) are typical for hypergiants rather than the classicalsupergiants. IRAS01005 +7910 is an example of spectral mimicry of a low masspost-AGB star masquerading as a massive hypergiant.

Spectral variability of the IR-source IRAS 01005+7910 optical component