  We introduce the first synthetic light-curve model set of Type IIP supernovae
exploded within circumstellar media in which the acceleration of the red
supergiant winds is taken into account. Because wind acceleration makes the
wind velocities near the progenitors low, the density of the immediate vicinity
of the red supergiant supernova progenitors can be higher than that
extrapolated by using a constant terminal wind velocity. Therefore, even if the
mass-loss rate of the progenitor is relatively low, it can have a dense
circumstellar medium at the immediate stellar vicinity and the early light
curves of Type IIP supernovae are significantly affected by it. We adopt a
simple beta velocity law to formulate the wind acceleration. We provide
bolometric and multicolor light curves of Type IIP supernovae exploding within
such accelerated winds from the combinations of three progenitors, 12 - 16
Msun; five beta, 1-5; seven mass-loss rates, 1e-5 - 1e-2 Msun/yr; and four
explosion energies, 0.5e51 - 2e51 erg. All the light curve models are available
at https://goo.gl/o5phYb. When the circumstellar density is sufficiently high,
our models do not show a classical shock breakout as a consequence of the
interaction with the dense and optically-thick circumstellar media. Instead,
they show a delayed 'wind breakout', substantially affecting early light curves
of Type IIP supernovae. We find that the mass-loss rates of the progenitors
need to be 1e-3 - 1e-2 Msun/yr to explain typical rise times of 5 - 10 days in
Type IIP supernovae assuming a dense circumstellar radius of 1e15 cm.
