This article has an erratum: [erratum]
Volume 521, October 2010
|Number of page(s)||4|
|Published online||19 October 2010|
Letter to the Editor
Averting the magnetic braking catastrophe on small scales: disk formation due to Ohmic dissipation
Department of Physics & Astronomy, The University of Western Ontario, 1151 Richmond St., London, ON, N6A 3K7, Canada e-mail: email@example.com, firstname.lastname@example.org
Accepted: 1 October 2010
We perform axisymmetric resistive MHD calculations that demonstrate that centrifugal disks can indeed form around Class 0 objects despite magnetic braking. We follow the evolution of a prestellar core all the way to near-stellar densities and stellar radii. Under flux-freezing, the core is braked and disk formation is inhibited, while Ohmic dissipation renders magnetic braking ineffective within the first core. In agreement with observations that do not show evidence for large disks around Class 0 objects, the resultant disk forms in close proximity to the second core and has a radius of only ≈ 10 early on. Disk formation does not require enhanced resistivity. We speculate that the disks can grow to the sizes observed around Class II stars over time under the influence of both Ohmic dissipation and ambipolar diffusion, as well as internal angular momentum redistribution.
Key words: magnetohydrodynamics (MHD) / protoplanetary disks / stars: formation / stars: magnetic field
© ESO, 2010
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