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Using a suite of 3D hydrodynamical simulations of star-forming molecularclouds, we investigate how the density probability distribution function (PDF)changes when including gravity, turbulence, magnetic fields, and protostellaroutflows and heating. We find that the density PDF is not lognormal whenoutflows and self-gravity are considered. Self-gravity produces a power-lawtail at high densities and the inclusion of stellar feedback from protostellaroutflows and heating produces significant time-varying deviations from alognormal distribution at the low densities. The simulation with outflows hasan excess of diffuse gas compared to the simulations without outflows, exhibitsincreased average sonic Mach number, and maintains a slower star formation rateover the entire duration of the run. We study the mass transfer between thediffuse gas in the lognormal peak of the PDF, the collapsing gas in thepower-law tail, and the stars. We find that the mass fraction in the power-lawtail is constant, such that the stars form out of the power-law gas at the samerate at which the gas from the lognormal part replenishes the power-law. Wefind that turbulence does not provide significant support in the dense gasassociated with the power-law tail. When including outflows and magnetic fieldsin addition to driven turbulence, the rate of mass transfer from the lognormalto the power-law, and then to the stars, becomes significantly slower,resulting in slower star formation rates and longer depletion times.

The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density PDF in Turbulent Star-Forming Clouds