The role of turbulent convection in the primitive solar nebula. I - Theory. II - Results

Details The role of turbulent convection in the primitive solar nebula. I - Theory. II - Results The role of turbulent convection in the primitive solar nebula. I - Theory. II - Results

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987icar...69..387c&link_type=abstract

Icarus (ISSN 0019-1035), vol. 69, March 1987, p. 387-457.

Computer Science

73

Convective Flow, Solar Corona, Stellar Evolution, Stellar Models, Turbulent Flow, Magnetohydrodynamic Stability, Solar Rotation

Scientific paper

A model of convective turbulence which takes radiative dissipation, rotation, and convective motion anisotropy into account, on the basis of a closure for the nonlinear interactions that employs the growth rates of hydrodynamic instabilities, is used to obtain a theoretical framework for modeling the primordial solar nebula. It is assumed that convection is the sole source of turbulence causing the solar nebula to evolve. Vertical structure equations in the thin disk approximation are developed and a detailed comparison with the previous solar nebula convective models of such workers as Lin et al. (1981, 1982) is undertaken. The present values for the turbulent efficiency are much lower and more sensitive to opacity and surface density, resulting in low turbulent speeds, a more massive disk, a lower accretion rate 'best value', and a longer characteristic dispersal time for the disk. It is concluded that convection may not be the dominant source of turbulence needed to evolve young solar/stellar nebulae.

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