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Magnetic fields are invoked as a key regulator of star formation at all
stages, from explaining the low efficiency of star formation in molecular
clouds to regulating star-disk interaction and outflows. I focus on magnetic
fields at various scales of the star formation process, with an emphasis
on the early phases. I review two key ideas of magnetic field regulated
fragmentation: turbulence accelerated star formation and two-stage fragmentation. Dense cores formed through the above processes are expected to exhibit hourglass magnetic field morphologies, and will eventually establish an inner region with a split monopole magnetic field configuration. In this situation, disk formation is prevented in the limit of flux freezing and an aligned rotator. I review some resolutions to this problem. Finally, I comment on the dual role of magnetic flux dissipation in enabling disk formation but also being limited enough to allow for outflows and eventual magnetic field line detachment.
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