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Star formation is inefficient. Recent advances in numerical simulations andtheoretical models of molecular clouds show that the combined effects ofinterstellar turbulence, magnetic fields and stellar feedback can explain thelow efficiency of star formation. The star formation rate is highly sensitiveto the driving mode of the turbulence. Solenoidal driving may be more importantin the Central Molecular Zone, compared to more compressive driving agents inspiral-am clouds. Both theoretical and observational efforts are underway todetermine the dominant driving mode of turbulence in different Galacticenvironments. New observations with ALMA, combined with other instruments suchas CARMA, JCMT and the SMA begin to reveal the magnetic field structure ofdense cores and protostellar disks, showing highly complex field geometrieswith ordered and turbulent field components. Such complex magnetic fields cangive rise to a range of stellar masses and jet/outflow efficiencies in densecores and protostellar accretion disks.

Star formation in cloud cores -- simulations and observations of dense molecular cores and the formation of solar mass stars