  We present a time-dependent, one-dimensional magnetically driven disk-wind
model based on magnetohydrodynamical (MHD) equations in the context of tidal
disruption events (TDEs). We assume that the disk is geometrically thin and
gas-pressure dominant and explicitly take into account magnetic braking as well
as turbulent viscosity by an extended alpha viscosity prescription. We find a
particular wind solution for a set of basic equations that satisfies the
necessary and sufficient conditions for vertically unbound MHD flows. The
solution demonstrates that the disk evolves with losing mass due to wind and
accretion from the initial Gaussian density distribution. We confirm that the
mass accretion rate follows the power law of time $t^{-19/16}$ at late times if
the wind is absent, which corresponds to the classical solution of Cannizzo et
al. (1990). We find that the mass accretion rate is steeper than the
$t^{-19/16}$ curve if the disk wind is present. This is because the wind
removes a significant fraction of the mass and angular momentum. Mass accretion
is further induced by magnetic braking, known as a wind-driven accretion
mechanism, resulting in more rapid decay with time in both the mass accretion
and loss rates. The ultraviolet (UV) luminosity is the highest among the
optical, UV, and X-ray luminosities from early to late evolutionary phases,
suggesting optical and X-ray emissions from the disk are observationally
insignificant due to magnetically driven winds in TDEs. Our model predicts that
late-time bolometric light curves steeper than $t^{-19/16}$ in UV-bright TDEs
potentially serve as compelling indicators for magnetically driven winds.
