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Powerful jets and outflows are launched from the protostellar disks aroundnewborn stars. These outflows carry enough mass and momentum to transform thestructure of their parent molecular cloud and to potentially control starformation itself. Despite their importance, we have not been able to fullyquantify the impact of jets and outflows during the formation of a starcluster. The main problem lies in limited computing power. We would have toresolve the magnetic jet-launching mechanism close to the protostar and at thesame time follow the evolution of a parsec-size cloud for a million years.Current computer power and codes fall orders of magnitude short of achievingthis. In order to overcome this problem, we implement a subgrid-scale (SGS)model for launching jets and outflows, which demonstrably converges andreproduces the mass, linear and angular momentum transfer, and the speed ofreal jets, with ~ 1000 times lower resolution than would be required withoutSGS model. We apply the new SGS model to turbulent, magnetized star clusterformation and show that jets and outflows (1) eject about 1/4 of their parentmolecular clump in high-speed jets, quickly reaching distances of more than aparsec, (2) reduce the star formation rate by about a factor of two, and (3)lead to the formation of ~ 1.5 times as many stars compared to the no-outflowcase. Most importantly, we find that jets and outflows reduce the average starmass by a factor of ~ 3 and may thus be essential for understanding thecharacteristic mass of the stellar initial mass function.

Modeling jet and outflow feedback during star cluster formation