论文标题
用外显子探测行星：开普勒-1708 B和开普勒1625 b的情况
Probing Planets with Exomoons: The Cases of Kepler-1708 b and Kepler-1625 b
论文作者
论文摘要
行星和月亮之间的潮汐相互作用可以洞悉宿主行星的特性。最近的Exomoon候选人Kepler-1708 B-I和Kepler-1625 B-I是海王星大小的卫星，绕着类似木星的行星旋转，并提供了应用此类方法的机会。我们表明，如果潮汐迁移时间大致等于这些系统的年龄，那么Planets Kepler-1708 B和Kepler-1625 B的潮汐耗散因子Q分别为〜$ 3 \ times10^5-3 \ times10^6 $和〜$ 1.5 \ $ 1.5 \ times10^times10^5-4 \ times10^5-4 \ times10^5-4 \ times10^5 $。在每种情况下，这些都与气体巨型行星的估计值一致。即使某些工作暗示了Kepler-1625 B-I的一个特别大的半轴轴，但我们发现，对于气体巨头来说，这意味着令人惊讶的Q〜2000，除非月球在本质上是其当前位置。对卫星最初的半隔轴的更详细的预测可以在Q上提供更好的约束，我们在这种情况下讨论了月球的形成场景。可以使用类似的参数，因为将来会发现更多的外族子来限制系外行星的内部特性。这对于在行星结构尚不确定的次音/超级半径间隙附近附近的系外行星特别有用。
The tidal interactions between a planet and moon can provide insight into the properties of the host planet. The recent exomoon candidates Kepler-1708 b-i and Kepler-1625 b-i are Neptune-sized satellites orbiting Jupiter-like planets and provide an opportunity to apply such methods. We show that if the tidal migration time is roughly equal to the age of these systems, then the tidal dissipation factor Q for the planets Kepler-1708 b and Kepler-1625 b have values of ~$3\times10^5-3\times10^6$ and ~$1.5\times10^5-4\times10^5$, respectively. In each case, these are consistent with estimates for gas giant planets. Even though some work suggests an especially large semimajor axis for Kepler-1625 b-i, we find that this would imply a surprisingly low Q~2000 for a gas giant unless the moon formed at essentially its current position. More detailed predictions for the moons' initial semimajor axis could provide even better constraints on Q, and we discuss the formation scenarios for a moon in this context. Similar arguments can be used as more exomoons are discovered in the future to constrain exoplanet interior properties. This could be especially useful for exoplanets near the sub-Neptune/super-Earth radius gap where the planet structure is uncertain.
