  1ES 1927+654 was known as a type 2 Seyfert galaxy, which exhibited drastic
variability recently in ultraviolet (UV)/optical and X-ray bands. An UV/optical
outburst was observed in the end of 2017, and it reached the peak luminosity
$\sim 50$ days later. The high-cadence observations showed a rapid X-ray flux
decline with complete disappearance of the power-law hard X-ray component when
the soft X-ray thermal emission reached its lowest level about $150$ days after
the UV/optical peak. The power law X-ray component reappeared with thermal
X-ray emission brightening from its lowest flux within next $\sim$ 100~days. We
assume an episodic accretion event taking place in the outer region of the disc
surrounding a central black hole (BH), which is probably due to a red giant
star tidally disrupted by the BH. The inner thin disc with corona is completely
swept by the accretion event when the gas reaches the innermost circular stable
orbit. The field threading the disrupted star is dragged inwards by the disc
formed after the tidal disruption event, which accelerates outflows from the
disc. The disc dimmed since a large fraction of the energy released in the disc
is tapped into the outflows. The accretion rate of the episodic accretion event
declines, and ultimately it turns out to be a thin disc, which is inefficient
for field advection, and the outflows are switched off. A thin disc with corona
reappears later after the outburst.
