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Shear instabilities in the dust layer of the solar nebula II. Different unperturbed states

机译：太阳星云II尘埃层的剪切不稳定性。不同的状态

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摘要

In the previous paper (Sekiya and Ishitsu, 2000), the shear instability in the dust layer of the solar nebula was investigated by using the constant Richardson number solution (Sekiya, 1998) as the unperturbed state, and the growth rate of the most unstable mode was calculated to be much less than the Keplerian angular velocity as long as the Richardson number was larger than 0.1. In this paper, we calculate the growth rate using different unperturbed states: (1) a sinusoidal density distribution, and (2) a constant density around the midplane with sinusoidal transition regions. An unperturbed state of this paper is considered to correspond to the first stage of shear instability that occurs as a result of dust settling in a laminar phase of the solar nebula. On the other hand, the unperturbed state of the previous paper corresponds to the quasi-equilibrium state (Sekiya, 1998) which is attained by the turbulent mixing. The results show that the growth rate is much larger than the Keplerian angular velocity, in contrast to the previous result.
机译：在先前的论文（Sekiya和Ishitsu，2000年）中，以恒定的Richardson数解（Sekiya，1998年）为扰动状态，研究了太阳星云尘埃层中的剪切失稳，最不稳定的增长率只要Richardson数大于0.1，就可以计算出模态比开普勒角速度小得多。在本文中，我们使用不同的扰动状态来计算增长率：（1）正弦密度分布，（2）具有正弦过渡区域的中平面周围的恒定密度。本文的未扰动状态被认为与剪切不稳定性的第一阶段相对应，该阶段是由于尘埃在太阳星云的层流相中沉降而发生的。另一方面，前一篇论文的无扰动状态对应于通过湍流混合获得的准平衡状态（Sekiya，1998）。结果表明，与以前的结果相反，增长率比开普勒角速度大得多。

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