Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348..730s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 348, Jan. 10, 1990, p. 730-737.
Astronomy and Astrophysics
Astrophysics
42
Accretion Disks, Astronomical Models, Solar Corona, Stellar Evolution, Stellar Mass Accretion, Angular Momentum, Cosmochemistry, Planetary Evolution, Thermochemistry
Scientific paper
The 'standard' accretion-disk model of the solar nebula is examined together with its basic equations, which are solved for the steady-state case. It is shown that, for this model of the solar nebula, the efficiency of mixing the products of thermochemical processing from small to large disk radii depends not on the magnitude of the eddy diffusivity but only on the ratio k between the eddy diffusivity and the eddy viscosity. In most cases, this ratio k is probably of order of unity or less, implying that most of the solar nebula was not contaminated by the consequences of thermochemical equilibria that were established at 'small' disk radii. It is noted that, while this condition is almost certainly satisfied if the physical process responsible for viscosity is thermal convection or waves, it has uncertain validity during the early phases of disk evolution where accretion-induced shear instabilities may dominate.
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