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
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原始太阳星云中湍流对流的作用。
DOI：
10.1016/0019-1035(87)90016-9
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发表时间：
1987
期刊：
影响因子：
--
通讯作者：
James B. Pollack
中科院分区：
文献类型：
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作者：
W. Cabot;V. Canuto;O. Hubickyj;James B. Pollack
提出了模拟原始太阳星云的理论框架，其中假设对流是导致星云演化的唯一湍流来源。我们使用一种新的对流湍流模型，该模型考虑了辐射耗散、旋转和对流运动各向异性的重要影响。该模型基于采用流体动力学不稳定性增长率的非线性相互作用的闭包，该过程允许人们计算对流以外的不稳定性的湍流系数。为这个新模型开发了薄盘近似中的垂直结构方程，并对先前的太阳星云对流模型进行了详细的比较和批评。数值结果将在后续论文中介绍。
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.