The role of turbulent convection in the primitive solar nebula: I. Theory |
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| Affiliation: | 1. Laboratoire de Géologie de Lyon, CNRS UMR 5276, University Claude Bernard Lyon 1, France;2. Laboratoire d''Ecologie des Hydrosystèmes Naturels et Anthropisés, CNRS UMR 5023, University Claude Bernard Lyon 1, France;3. Laboratoire de Minéralogie et Cosmochimie du Muséum, CNRS–MNHN UMR 7202, Paris, France;1. The Southern Branch of the P.P. Shirshov Institute of Oceanology RAS, Gelendzhik, Krasnodar region, Russia;2. P.P. Shirshov Institute of Oceanology RAS, Nakhimovski av., Moscow, Russia;3. Laboratorio di Fisiologia delle Alghe e delle Piante, Dipartimento di Scienze della Vita e dell''Ambiente, Università Politecnica delle Marche, Ancona, Italy;4. STU-UNIVPM Joint Algal Research Center, Shantou, China;5. Institute of Microbiology, Academy of Sciences of the Czech Republic, Algatech, Trebon, Czech Republic;6. National Research Council, Institute of Marine Science ISMAR, Venezia, Italy |
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| Abstract: | The theoretical framework for modeling the primordial solar nebula is presented in which convection is assumed to be the sole source of turbulence that causes the nebula to evolve. We use a new model of convective turbulence that takes into account the important effects of radiative dissipation, rotation, and anisotropy of convective motions. This model is based on a closure for the nonlinear interactions that employs the growth rates of hydrodynamic instabilities, a procedure that allows one to compute turbulence coefficients for instabilities other than convection. The vertical structure equations in the thin-disk approximation are developed for this new model, and a detailed comparison and critique of previous convective models of the solar nebula are presented. Numerical results are presented in a subsequent paper. |
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