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The star-forming efficiency of dense gas is thought to be set within cores byoutflow and radiative feedback. We use magneto-hydrodynamic simulations toinvestigate the relation between protostellar outflow evolution, turbulence andstar formation efficiency. We model the collapse and evolution of isolateddense cores for $\gtrsim$ 0.5 Myr including the effects of turbulence,radiation transfer, and both radiation and outflow feedback from formingprotostars. We show that outflows drive and maintain turbulence in the coreenvironment even with strong initial fields. The star-formation efficiencydecreases with increasing field strength, and the final efficiencies are$15-40$\%. The Stage 0 lifetime, during which the protostellar mass is lessthan the dense envelope, increases proportionally with the initial magneticfield strength and ranges from $\sim 0.1-0.4$ Myr. The average accretion rateis well-represented by a tapered turbulent core model, which is a function ofthe final protostellar mass and is independent of the magnetic field strength.By tagging material launched in the outflow, we demonstrate that the outflowentrains about $3$ times the actual launched gas mass, a ratio that remainsroughly constant in time regardless of the initial magnetic field strength.However, turbulent driving increases for stronger fields since momentum is moreefficiently imparted to non-outflow material. The protostellar outflow momentumis highest during the first 0.1 Myr and declines thereafter by a factor of$\gtrsim 10$ as the accretion rate diminishes.

Impact of Protostellar Outflows on Turbulence and Star Formation Efficiency in Magnetized Dense Cores