论文标题
由于惯性波造成的潮汐耗散可以解释太阳能二进制的循环周期
Tidal dissipation due to inertial waves can explain the circularization periods of solar-type binaries
论文作者
论文摘要
潮汐耗散是为了使轨道循环并同步太阳能近距离二进制恒星的旋转，但是造成的机制尚未完全了解。先前的工作表明，需要对各种恒星种群中观察到的循环周期（$ p_ \ mathrm {Circ} $）解释观察到的循环周期（$ p_ \ mathrm {Circ} $）的显着增强，并且随着年龄的增长。这部分基于以下普遍的信念，即太阳能恒星中潮汐耗散的主要机制是作用于对流信封中平衡潮汐的湍流粘度。在本文中，我们研究了潮汐耗散在其演变后旋转太阳能恒星的对流和辐射带中。我们研究了潮汐耗散的平衡，并结合了最新流体动力学模拟和惯性波（动态潮汐）耗散的频率依赖性有效粘度，采用了频率平均形式主义，以说明恒星的现实结构。我们证明，观察到的二进制循环周期可以通过对流信封中的惯性波（动态潮汐）耗散来解释。在预序序列阶段，这种机制特别有效，但是如果自旋接近同步，它也可以在主序列上工作。由于这种机制，预测的$ p_ \ mathrm {circ} $随着观察结果而增加。我们还证明，即使在前序列序列中，基于我们对这些机制的最佳理解，即使在预先序列序列中，平衡潮水和内部重力波耗散也不可能解释观察到的$ p_ \ mathrm {Circ} $。最后，我们主张对由于惯性波造成的潮汐耗散的恒星种群的更现实的动力学研究。
Tidal dissipation is responsible for circularizing the orbits and synchronizing the spins of solar-type close binary stars, but the mechanisms responsible are not fully understood. Previous work has indicated that significant enhancements to the theoretically-predicted tidal dissipation rates are required to explain the observed circularization periods ($P_\mathrm{circ}$) in various stellar populations, and their evolution with age. This was based partly on the common belief that the dominant mechanism of tidal dissipation in solar-type stars is turbulent viscosity acting on equilibrium tides in convective envelopes. In this paper we study tidal dissipation in both convection and radiation zones of rotating solar-type stars following their evolution. We study equilibrium tide dissipation, incorporating a frequency-dependent effective viscosity motivated by the latest hydrodynamical simulations, and inertial wave (dynamical tide) dissipation, adopting a frequency-averaged formalism that accounts for the realistic structure of the star. We demonstrate that the observed binary circularization periods can be explained by inertial wave (dynamical tide) dissipation in convective envelopes. This mechanism is particularly efficient during pre-main sequence phases, but it also operates on the main sequence if the spin is close to synchronism. The predicted $P_\mathrm{circ}$ due to this mechanism increases with main-sequence age in accord with observations. We also demonstrate that both equilibrium tide and internal gravity wave dissipation are unlikely to explain the observed $P_\mathrm{circ}$, even during the pre-main sequence, based on our best current understanding of these mechanisms. Finally, we advocate more realistic dynamical studies of stellar populations that employ tidal dissipation due to inertial waves.
