晚型双星的圆化时标
The circularization timescales of late-type binary stars
摘要：
我们研究了Terquem（2021）提出的计算快潮汐和对流之间能量交换速率$D_R$的形式主义的结果，并将其应用。在以前的工作中，为了耗散潮汐能，假定$D_R$（与对流速度的梯度成比例）为正。在这里，我们认为，即使能量是间歇性地从对流转移到潮汐，它必须最终返回对流流和有效地输送到恒星表面的对流时间尺度。这与强制执行$D_R>0$是一致的，但限制性要小得多。我们的主要结果是晚型双星的圆化时标的计算，考虑到完整的恒星结构的时间演化。我们发现，循环是非常有效的PMS阶段期间，效率低下的MS期间，并再次有效时，明星接近RGB。这些结果比以前的理论更符合观测。我们也适用于我们的形式主义，以热彗星，并发现，潮汐耗散在木星质量的行星产生一个循环的时间尺度为1 Gyr的轨道周期为3 d，也在良好的整体协议与观测。这里的方法是新颖的，该理论在解决长期存在的时间尺度难题方面的明显成功是引人注目的。
英文摘要：
We examine the consequences of, and apply, the formalism developed in Terquem (2021) for calculating the rate $D_R$ at which energy is exchanged between fast tides and convection. In this previous work, $D_R$ (which is proportional to the gradient of the convective velocity) was assumed to be positive in order to dissipate the tidal energy. Here we argue that, even if energy is intermittently transferred from convection to the tides, it must ultimately return to the convective flow and transported efficiently to the stellar surface on the convective timescale. This is consistent with, but much less restrictive than, enforcing $D_R>0$. Our principle result is a calculation of the circularization timescale of late-type binaries, taking into account the full time evolution of the stellar structure. We find that circularization is very efficient during the PMS phase, inefficient during the MS, and once again efficient when the star approaches the RGB. These results are in much better agreement with observations than earlier theories. We also apply our formalism to hot Jupiters, and find that tidal dissipation in a Jupiter mass planet yields a circularization timescale of 1 Gyr for an orbital period of 3 d, also in good overall agreement with observations. The approach here is novel, and the apparent success of the theory in resolving longstanding timescale puzzles is compelling.
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