膨胀和收缩的热行星：已知凌日行星的耦合潮汐和热演化
Inflating and Deflating Hot Jupiters: Coupled Tidal and Thermal Evolution of Known Transiting Planets
摘要：
我们用耦合轨道潮汐演化和热演化的行星演化模型研究了近距离巨行星的半径演化。对于45个过境系统，我们计算了一个大的网格的冷却/收缩路径的时间向前，从一个大的相空间的初始半长轴和偏心率。给定给定行星当前时间的观测约束（半长轴、偏心率和系统年龄），我们找到符合这些约束的可能进化路径，并将计算出的半径与观测值进行比较。我们发现，潮汐演变有两个影响。首先，行星在较大的半长轴上开始演化，使它们在早期更有效地收缩。其次，潮汐加热可以显着膨胀的半径时，轨道被圆化，但这种影响的半径是短暂的。轨道的圆化过程通常会持续很长一段时间，而半长轴则会缓慢减小。我们可以用我们的耦合模型重现一些以前无法解释的大半径系统，如HAT-P-7，HAT-P-9，WASP-10和XO-4。这增加了我们可以匹配半径的行星的数量，从24（45）到我们标准情况下的35，但对于其中一些系统，我们需要在当前半径膨胀时代的特殊时间观察它们。这是一个关注的可行性潮汐膨胀的一般机制，以解释大多数膨胀半径。此外，大的初始偏心率必须是常见的。我们还研究了模型的演变，有一个地板上的偏心率，可能是由于一个扰动。在这种情况下，我们匹配WASP-12 b的极大半径。（节录）
英文摘要：
We examine the radius evolution of close-in giant planets with a planet evolution model that couples the orbital-tidal and thermal evolution. For 45 transiting systems, we compute a large grid of cooling/contraction paths forward in time, starting from a large phase space of initial semi-major axes and eccentricities. Given observational constraints at the current time for a given planet (semi-major axis, eccentricity, and system age) we find possible evolutionary paths that match these constraints, and compare the calculated radii to observations. We find that tidal evolution has two effects. First, planets start their evolution at larger semi-major axis, allowing them to contract more efficiently at earlier times. Second, tidal heating can significantly inflate the radius when the orbit is being circularized, but this effect on the radius is short-lived thereafter. Often circularization of the orbit is proceeded by a long period while the semi-major axis slowly decreases. Some systems with previously unexplained large radii that we can reproduce with our coupled model are HAT-P-7, HAT-P-9, WASP-10, and XO-4. This increases the number of planets for which we can match the radius from 24 (of 45) to as many as 35 for our standard case, but for some of these systems we are required to be viewing them at a special time around the era of current radius inflation. This is a concern for the viability of tidal inflation as a general mechanism to explain most inflated radii. Also, large initial eccentricities would have to be common. We also investigate the evolution of models that have a floor on the eccentricity, as may be due to a perturber. In this scenario we match the extremely large radius of WASP-12b. (Abridged)
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