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Observations of nearby molecular clouds detect "shells", which are likelycaused by winds from young main sequence stars. However, the progenitors ofthese observed features are not well characterized and the mass-loss ratesinferred from the gas kinematics are several orders of magnitude greater thanthose predicted by atomic line-driven stellar wind models. We usemagnetohydrodynamic simulations to model winds launching within turbulentmolecular clouds and explore the impact of wind properties on cloud morphologyand turbulence. We find that winds do not produce clear features in turbulentstatistics such as the Fourier spectra of density and momentum but do impactthe Fourier velocity spectrum. The density and velocity distribution functions,especially as probed by CO spectral lines, strongly indicate the presence andinfluence of winds. We show that stellar mass-loss rates for individual starsmust be $\dot m_w \gtrsim 10^{-7}$ Msun yr$^{-1}$, similar to those estimatedfrom observations, to reproduce shell properties. Consequently, we concludethat B and A-type main sequence stars have mass-loss rates several orders ofmagnitude larger that those predicted by models or that young stars are morevariable than expected due to magnetic activity or accretion.

Impact of Winds from Intermediate-Mass Stars on Molecular Cloud Structure and Turbulence