Dead Zone Accretion Flows in Protostellar Disks

Details Dead Zone Accretion Flows in Protostellar Disks Dead Zone Accretion Flows in Protostellar Disks

2008-04-17

arxiv.org/abs/0804.2916v1

Astronomy and Astrophysics

Astrophysics

12 pages, 4 figures

Scientific paper

10.1086/589540

Planets form inside protostellar disks in a dead zone where the electrical resistivity of the gas is too high for magnetic forces to drive turbulence. We show that much of the dead zone nevertheless is active and flows toward the star while smooth, large-scale magnetic fields transfer the orbital angular momentum radially outward. Stellar X-ray and radionuclide ionization sustain a weak coupling of the dead zone gas to the magnetic fields, despite the rapid recombination of free charges on dust grains. Net radial magnetic fields are generated in the magneto-rotational turbulence in the electrically conducting top and bottom surface layers of the disk, and reach the midplane by Ohmic diffusion. A toroidal component to the fields is produced near the midplane by the orbital shear. The process is similar to the magnetization of the Solar tachocline. The result is a laminar, magnetically-driven accretion flow in the region where the planets form.

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