  An origin of the Optical/UV radiation from tidal disruption events (TDEs) has
recently been discussed for different scenarios, but observational support is
generally missing. In this Letter, we test applicability of the `Wind-Driven
model' (Uno & Maeda 2020) to a sample of UV/Optical TDEs. With the model, we
aim to derive the physical properties of the Optical/UV TDEs, such as mass-loss
rates and characteristic radii. The model assumes optically thick continuous
outflows like stellar winds, and one key question is how the wind-launched
radius is connected to physical processes in TDEs. As one possibility, through
a comparison between the escape velocities estimated from their black-hole
masses and the wind velocities estimated from observed line widths, we propose
that the outflow is launched from the self-interaction radius ($R_{\rm SI}$)
where the stellar debris stretched by the tidal force intersects; we show that
the escape velocities at $R_{\rm SI}$ are roughly consistent with the wind
velocities. By applying the model to a sample of Optical/UV TDE candidates, we
find that explosive mass ejections ($\gtrsim 10 ~M_{\odot}{\rm yr^{-1}}$) from
$R_{\rm SI}$ ($\sim 10^{14}{\rm ~cm}$) can explain the observed properties of
TDEs around peak luminosity. We also apply the same framework to a peculiar
transient, AT2018cow. The model suggests that AT2018cow is likely a TDE induced
by an intermediate-mass black hole ($M_{\rm BH} \sim 10^{4}~M_{\odot}$).
