On a new formulation for energy transfer between convection and fast tides with application to giant planets and solar type stars
On a new formulation for energy transfer between convection and fast tides with application to giant planets and solar type stars
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对流和快潮之间能量转移的新公式应用于巨行星和太阳型恒星
DOI：
10.1093/mnras/stab224
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发表时间：
2021
影响因子：
4.8
通讯作者：
C. Terquem
中科院分区：
文献类型：
--
作者：
C. Terquem
所有关于潮汐与对流相互作用的研究都假定大尺度潮汐可以被描述为一个由小尺度脉动对流涡旋阻尼的平均切变流。对流雷诺应力的计算采用混合长度理论，占一个急剧抑制耗散周转时间尺度大于潮汐周期。这产生的潮汐耗散率几个数量级太小，无法解释晚型双星的循环周期或巨行星的潮汐耗散因子。在这里，我们认为，上述描述是不一致的，因为波动和平均流量应根据时间尺度，而不是在空间尺度上，他们的变化。因此，标准的图像应该颠倒过来，波动是潮汐振荡和最大的对流涡旋提供的平均切变流。我们假设能量是局部转移的潮汐对流。使用这个假设，我们得到的值的潮汐Q因子的木星和土星和循环周期的前主序星的二进制与观测结果吻合得很好。然而，用平衡潮汐近似得到的时间尺度仍然是晚型双星的圆化周期的40倍。对于这些系统，在速跃层或在对流带的底部剪切可能是潮汐耗散的主要原因。
All the studies of the interaction between tides and a convective flow assume that the large-scale tides can be described as a mean shear flow that is damped by small-scale fluctuating convective eddies. The convective Reynolds stress is calculated using mixing length theory, accounting for a sharp suppression of dissipation when the turnover time-scale is larger than the tidal period. This yields tidal dissipation rates several orders of magnitude too small to account for the circularization periods of late-type binaries or the tidal dissipation factor of giant planets. Here, we argue that the above description is inconsistent, because fluctuations and mean flow should be identified based on the time-scale, not on the spatial scale, on which they vary. Therefore, the standard picture should be reversed, with the fluctuations being the tidal oscillations and the mean shear flow provided by the largest convective eddies. We assume that energy is locally transferred from the tides to the convective flow. Using this assumption, we obtain values for the tidal Q factor of Jupiter and Saturn and for the circularization periods of pre-main-sequence binaries in good agreement with observations. The time-scales obtained with the equilibrium tide approximation are however still 40 times too large to account for the circularization periods of late-type binaries. For these systems, shear in the tachocline or at the base of the convective zone may be the main cause of tidal dissipation.
太阳型恒星中心附近的内波破碎和潮汐耗散
DOI：
10.1111/j.1365-2966.2010.16400.x
发表时间：
2010
影响因子：
4.8
作者：
Barker A
通讯作者：
Barker A
演化中的低质量恒星和太阳型恒星的潮汐耗散以及对行星轨道衰变的预测
影响因子：
4.8
作者：
Barker A
通讯作者：
Barker A
作用于平衡潮汐流的对流湍流粘度：有效粘度的新频率缩放
影响因子：
4.8
作者：
Duguid C
通讯作者：
Duguid C