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Can non ideal magnetohydrodynamics solve the magnetic braking catastrophe?

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Figure

Figure 1. Top to bottom: grain charge, charged species number densities,density (top scale), and the bottom ticks correspond to number density (bot-tom scale)
Figure 2. Face-on gas column density using ideal MHD. The initial rotation is counterclockwise and the initial magnetic field is directed out of the page (i.e.B0 · �0 > 0)
Figure 3. Disc properties for the ideal (left) and non-ideal (right) MHD models with ∼3 × 105 particles in the sphere
Figure 5. Edge-on gas column density using ideal MHD and zoomed out to (3000 au)2 and using a density range shifted down by a factor of 10 to visualizethe full extent of the outflows launched shortly after the collapse (t ≈ 1.02 tff) in the magnetic models
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