Structure Formation in Planetary Disk and Laboratory Plasma

Physics – Plasma Physics

Scientific paper

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Scientific paper

The shear flow instabilities under the presence of magnetic fields in the protoplanetary disk can greatly facilitate the formation of density structures that serve prior to the onset of the gravitational Jeans instability as a seed for the faster formation of planetesimals. Such a process may explain several puzzles in the planetary genesis. We evaluate the effects of the Parker, magnetorotational, and kinematic dynamo instabilities, and calculate the mass spectra of coagulated density structures by the above mechanism in the radial direction for two typical models. The mass spectrum of the magnetorotational instability may describe the origin of giant planets away from central star. Our local three-dimentional MHD simulation indicates that the coupling of those instabilities creates spiral arms and gas blobs in the accretion disk, reinforcing our theory. Such a mechanism for the early structure formation may be tested in a laboratory. The recent progress in experiments invloving shear flows in tokamak and laser plasmas may become a key in this regard. * The work is supported by NSF and DoE.

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