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Fig. 11


Evidence for disk formation. Top panel: column density profile. The system is Toomre-unstable, and breaks up into a ring in the resistive model (solid line), but not in the flux-frozen model (dotted line). Middle panel: infall profile. Infall is stopped in the resistive model (solid line), in innermost region where a centrifugal disk forms, but not in the flux-frozen model (dotted line). Bottom panel: ratio of centrifugal over gravitational acceleration. In the resistive model, centrifugal balance is achieved. In contrast, catastrophic magnetic braking occurs for the flux-frozen model, the centrifugal support drops to negligible values and the first core is spun down drastically.

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