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首页> 外文期刊>Earth, planets and space: EPS >Shear instabilities in the dust layer of the solar nebula I. The linear analysis of a non-gravitating one-fluid model without the Coriolis and the solar tidal forces
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Shear instabilities in the dust layer of the solar nebula I. The linear analysis of a non-gravitating one-fluid model without the Coriolis and the solar tidal forces

机译：太阳星云尘埃层中的剪切不稳定性I.没有科里奥利和太阳潮汐力的非重力单流体模型的线性分析

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As dust aggregates settled toward the midplane of the solar nebula, a thin dust layer was formed. The rotational velocity was a function of the distance from the midplane in this layer, and the shear induced turbulence might occur, which prevented the dust aggregates from settling further toward the midplane. Thus, it was difficult for the dust density on the midplane to exceed the critical density of the gravitational stability. In this paper, the linear analysis of the shear instability is made under the following assumptions: The self-gravity, the solar tidal force (thus the Keplerian shear), and the Coriolis force are neglected; the unperturbed state has a constant Richardson's number in the dust layer; further we restrict ourselves to the case where dust aggregates are small enough, and a mixture of dust and gas is treated as one fluid. Numerical results show that the growth rate of the most unstable mode is much less than the Keplerian angular frequency, as long as the Richardson number is larger than 0.1.
机译：当尘埃聚集到太阳星云的中平面时，形成了一层薄薄的尘埃层。旋转速度是该层中距中平面的距离的函数，并且可能会发生由剪切引起的湍流，这会阻止粉尘聚集进一步向中平面沉降。因此，中平面上的尘埃密度难以超过重力稳定性的临界密度。在以下假设中，对剪力不稳定性进行了线性分析：忽略了自重，太阳潮汐力（即Keplerian剪力）和科里奥利力;不受干扰的状态在尘埃层中具有恒定的理查森数。此外，我们将自己局限于粉尘聚集体足够小的情况，并且粉尘和气体的混合物被视为一种流体。数值结果表明，只要理查森数大于0.1，最不稳定模的增长率远小于开普勒角频率。

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