Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1311t&link_type=abstract
American Astronomical Society, DPS meeting #38, #13.11; Bulletin of the American Astronomical Society, Vol. 38, p.507
Astronomy and Astrophysics
Astronomy
Scientific paper
Magnetorotational turbulence in the Solar nebula is explored using 3-D resistive MHD computer calculations. The coupling between gas and magnetic fields is found by solving a simplified time-dependent ionization and recombination reaction network in each grid cell. Interstellar cosmic rays ionize the top and bottom surfaces of the nebula. When the cross section of the embedded dust grains is decreased sufficiently by coagulation or settling, recombination occurs mainly in the gas phase and the timescales for recombination and turbulent mixing are similar, so that the exchange of material between the surface and interior can potentially alter the thickness of the layer coupled to the magnetic fields. However the mixing proves too slow to carry ions and electrons to the midplane before they recombine. The majority of the column mass at 1 AU remains non-turbulent and decoupled from the fields. Under these conditions, gas and solids will accumulate in the quiescent interior, providing favorable conditions for the growth of planetesimals.
The Jet Propulsion Laboratory is operated by the California Institute of Technology under contract to NASA.
Dziourkevitch Natalia
Sano Takayoshi
Turner Neal James
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