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We present three Orion simulations of star cluster formation in a 1000 Msun,turbulent molecular cloud clump, including the effects of radiative transfer,protostellar outflows, and magnetic fields. Our simulations all useself-consistent turbulent initial conditions and vary the mean mass-to-fluxratio relative to the critical value over 2, 10, and infinity to gauge theinfluence of magnetic fields on star cluster formation. We find, in goodagreement with previous studies, that magnetic fields of typically observedstrengths lower the star formation rate by a factor of 2.4 and reduce theamount of fragmentation by a factor of 2 relative to the zero-field case. Wealso find that the field increases the characteristic sink particle mass, againby a factor of 2.4. The magnetic field also increases the degree of clusteringin our simulations, such that the maximum stellar densities in the strong fieldcase are higher than the others by again a factor of 2. This clustering tendsto encourage the formation of multiple systems, which are more common in therad-MHD runs than the rad-hydro run. The companion frequency in our simulationsis consistent with observations of multiplicity in Class I sources,particularly for the strong field case. Finally, we find evidence of primordialmass segregation in our simulations reminiscent of that observed in starclusters like the Orion Nebula Cluster.

Star Cluster Formation in Turbulent, Magnetized Dense Clumps with Radiative and Outflow Feedback