The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density Probability Distribution Function in Turbulent Star-forming Clouds

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