论文标题
搜索整个开普勒数据。 ii。 FGK恒星的发生率估计值
Searching the Entirety of Kepler Data. II. Occurrence Rate Estimates for FGK Stars
论文作者
论文摘要
我们介绍了估计的外部发生率，该行星在0.5至16 $ r _ {\ bigoplus} $和0.78至400天之间的贝叶斯计算估计，旋转FGK DWARF恒星。我们的结果基于一个独立的行星目录，该目录是根据我们对开普勒任务观察到的所有约20万颗恒星的搜索，并在GAIA DR2融合的恒星Radii中补充了精确的行星半径。我们考虑了数据中的检测和审查效率，行星半径不确定性以及可靠性的数据中的类似于Transit的噪声信号的可靠性。通过分析我们的FGK发生率以及分离F-，G-和K型恒星后计算的率，我们探索了对恒星有效温度，行星半径和轨道周期的依赖性。我们揭示了〜1.5至2 $ r _ {\ bigoplus} $之间光蒸发驱动的“半径差距”的新特征，这表明先前在$ p $ <100天之前揭示的双峰分布仅在狭窄的轨道范围内存在，在较狭窄的范围内，在上面，在哪些占主导地下和下方是超越哪个超级等级的超级等级。最后，我们提供了“ eta-earth”值的几个估计值 - 潜在的可居住的岩石行星绕着阳光恒星的恒星的频率。对于尺寸为0.75-1.5 $ r _ {\ bigoplus} $的行星，在G型星周围的保守定义的可居住区（0.99-1.70 au）中，我们将上限（84.1个百分位数）<0.18个星球，每颗恒星每颗恒星。
We present exoplanet occurrence rates estimated with approximate Bayesian computation for planets with radii between 0.5 and 16 $R_{\bigoplus}$ and orbital periods between 0.78 and 400 days, orbiting FGK dwarf stars. We base our results on an independent planet catalogue compiled from our search of all ~200,000 stars observed over the Kepler mission, with precise planetary radii supplemented by Gaia DR2-incorporated stellar radii. We take into account detection and vetting efficiency, planet radius uncertainty, and reliability against transit-like noise signals in the data. By analyzing our FGK occurrence rates as well as those computed after separating F-, G-, and K-type stars, we explore dependencies on stellar effective temperature, planet radius, and orbital period. We reveal new characteristics of the photoevaporation-driven "radius gap" between ~1.5 and 2 $R_{\bigoplus}$, indicating that the bimodal distribution previously revealed for $P$ < 100 days exists only over a much narrower range of orbital periods, above which sub-Neptunes dominate and below which super-Earths dominate. Finally, we provide several estimates of the "eta-Earth" value -- the frequency of potentially habitable, rocky planets orbiting Sun-like stars. For planets with sizes 0.75 - 1.5 $R_{\bigoplus}$ orbiting in a conservatively defined habitable zone (0.99 - 1.70 AU) around G-type stars, we place an upper limit (84.1th percentile) of <0.18 planets per star.
