双星中行星动力学的再研究：演化时标和早期恒星演化的影响
Revisiting the dynamics of planets in binaries: evolutionary timescales and the effect of early stellar evolution
摘要：
双星中行星的发现是行星研究中最有趣的成果之一。随着越来越多的发现，人们对描述它们的形成、长期演化和潜在的可居住性也越来越感兴趣。在这项工作中，我们重新审视的动力学的行星在S型双星系统。为此，我们开发明确的公式，再加上广义相对论修正和非保守相互作用的世俗八极哈密顿量。我们在一个开源软件包\texttt{SecDev3B}中实现了这些公式，该软件包可用于重现我们的结果或测试模型的改进版本。为了验证这一点，我们研究了恒星演化前主序星阶段S型双星的长期动力学演化。在这一阶段，恒星半径在类似于长期时间尺度的时间尺度上发生了显着变化。我们假设，当近距离接触的行星和它的宿主恒星发生（例如通过Lidov-Kozai效应），在长期的形式主义加上恒星半径的变化的特殊性可能会改变显着的动力学演化。我们研究了著名的双行星HD 80606 b，发现需要一个八极展开的保守哈密顿量，以正确地预测其动力学演化。我们还应用的动力学模型，丰富的结果来自恒星演化模型，以证明在S型系统周围的低质量恒星，相对较高的倾角（$\itot\ge 60^\circ$），中等偏心率（$0.2\le e\le 0.4$）和行星位于1 AU，恒星半径的演变，在最初的几百万年，改变显着的动力学演化的时间尺度。
英文摘要：
The discovery of planets in binaries is one the most interesting outcomes of planetary research. With the growing number of discoveries has also grown the interest on describing their formation, long-term evolution and potential habitability. In this work we revisit the dynamics of planets in S-type binary systems. For that purpose we develop explicit formulas for the secularized octupolar Hamiltonian, coupled with general relativistic corrections and non-conservative interactions. We implemented those formulas in an open-source package \texttt{SecDev3B}, that can be used to reproduce our results or test improved versions of the models. In order to test it, we study the long-term dynamical evolution of S-type binary planets during the pre-main-sequence phase of stellar evolution. During that phase, stellar radius significantly changes in timescales similar to secular timescales. We hypothesize that when close-encounters between the planet and its host star happens (e.g. via Lidov-Kozai effect), particularities in the secular formalism plus changes in stellar radius may alter significantly the dynamical evolution. We study the well-known binary planet HD 80606b and found that an octupolar expansion of the conservative Hamiltonian is required to properly predict its dynamical evolution. We also apply the dynamical model, enriched with results coming from stellar evolutionary models, to demonstrate that in S-type systems around low-mass stars, with relative high inclinations ($\itot\ge 60^\circ$), moderate eccentricities ($0.2\le e\le 0.4$) and planets located around 1 AU, the evolution of stellar radius during the first few hundreds of Myr, alters significantly the timescales of dynamical evolution.
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