Fast Tides in Slow Stars: The Efficiency of Eddy Viscosity
Fast Tides in Slow Stars: The Efficiency of Eddy Viscosity
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DOI：
10.1086/304505
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发表时间：
1997-01
期刊：
影响因子：
--
通讯作者：
J. Goodman;S. P. Oh
中科院分区：
文献类型：
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作者：
J. Goodman;S. P. Oh
湍流粘性被认为可以使双星轨道循环和同步，并抑制恒星的振荡。较老的双星似乎是循环到更长的周期，这表明循环在主序阶段进行。当潮汐周期短于最大涡旋的周转时间时，湍流粘性被部分抑制。然而，压制的程度存在争议。我们重新审视这两个信念通过（1）直接微扰计算，线性化的流体方程的湍流背景下;（2）数值积分的混沌动力系统的周期性强迫。我们发现，快速潮汐的消散被严重抑制。即使当我们忽略这种抑制，我们得出结论，一些机制以外的湍流对流循环太阳型双星。
Turbulent viscosity is believed to circularize and synchronize binary orbits and to damp stellar oscillations. Older binaries appear to be circular out to longer periods, which indicates that circularization proceeds during the main-sequence phase. It is also believed that when the tidal period is shorter than the turnover time of the largest eddies, turbulent viscosity is partially suppressed. The degree of suppression, however, is disputed. We reexamine both of these beliefs via (1) direct perturbative calculations, linearizing the fluid equations on a turbulent background; and (2) numerical integration of a chaotic dynamical system subject to periodic forcing. We find that dissipation of rapid tides is severely suppressed. Even when we disregard this suppression, we conclude that some mechanism other than turbulent convection circularizes solar-type binaries.