  Observations of nearby molecular clouds detect "shells", which are likely
caused by winds from young main sequence stars. However, the progenitors of
these observed features are not well characterized and the mass-loss rates
inferred from the gas kinematics are several orders of magnitude greater than
those predicted by atomic line-driven stellar wind models. We use
magnetohydrodynamic simulations to model winds launching within turbulent
molecular clouds and explore the impact of wind properties on cloud morphology
and turbulence. We find that winds do not produce clear features in turbulent
statistics such as the Fourier spectra of density and momentum but do impact
the Fourier velocity spectrum. The density and velocity distribution functions,
especially as probed by CO spectral lines, strongly indicate the presence and
influence of winds. We show that stellar mass-loss rates for individual stars
must be $\dot m_w \gtrsim 10^{-7}$ Msun yr$^{-1}$, similar to those estimated
from observations, to reproduce shell properties. Consequently, we conclude
that B and A-type main sequence stars have mass-loss rates several orders of
magnitude larger that those predicted by models or that young stars are more
variable than expected due to magnetic activity or accretion.
