  We discuss a revision of accretion activity and kinematics of the enigmatic
isolated UX Ori type star RZ Psc. Previously, RZ Psc was known to possess only
spectroscopic signatures of outflow in the low-excitation lines of alkali
metals. The archival high-resolution spectra reveal a short-lived episode of
magnetospheric accretion in the system observed via inverse P Cyg profiles at
the H$\alpha$ and CaII 8542 $\unicode{x212B}$ lines. The simultaneous presence
of accretion and outflow signatures at CaII 8542 $\unicode{x212B}$ is
suggestive of an accretion-driven origin of the RZ Psc wind. We argue that RZ
Psc experiences matter ejection via the magnetic propeller mechanism but
variable accretion episodes allow it to sometimes move in the magnetospheric
accretion regime. The presence of the weak accretion in the system is also
supported by the radiation of the hot accretion spot on the stellar surface
observed spectroscopically at the deep photometric minimum of the star. The
Galactic motion of RZ Psc calculated with new GAIA DR2 astrometric data
suggests possible membership in Cas-Tau OB association with an age of
$t=20^{+3}_{-5}$ Myr.
