  The similarity in physical conditions in winds of low-mass post-asymptotic
giant branch stars and evolved massive stars leads to the appearance of an
interesting phenomenon of spectral mimicry. Due to that the discovery of every
new star with Wolf--Rayet spectrum requires special study of its evolutionary
status before it may be included in the list of Galactic Wolf--Rayet (WR)
stars. A couple of years ago LAMOST J040901.83+323955.6 (hereafter J0409+3239)
was selected as a WR star in LAMOST spectroscopic database by machine learning
methods. In this work we investigated its evolutionary status. Analyzing the
spatial location of J0409+3239, in the Galaxy and its position in the
color-magnitude diagram we concluded what J0409+3239, is instead a low mass
object with WR phenomenon. Its luminosity is $L*=1000 L_\odot$ and effective
temperature $T_{\rm eff}$=40,000 K. Using new and archival photometric data we
detected irregular variability on time scales from hours to tens of days with
amplitude up to $\approx0.2$ mag. Comparison of the spectrum obtained in 2022
with the one from 2014 also shows an evidence of spectral variability. The
absence of clearly detected circumstellar nebula does not allow to classify
J0409+3239, as [WR], i.e. a central star of planetary nebula (CSPN). However,
its position in Hertzsprung--Russell diagram suggests that J0409+3239, is a low
mass star caught in rare transitional phase to CSPN. Estimation of J0409+3239,
mass based on evolutionary tracks shows that it is less than $0.9~M_\odot$, and
thus the age of the Galaxy is barely enough for the star to evolve to its
current stage.
