论文标题
一个简化的光动力学模型，用于低分子多传输系统中行星质量测定
A Simplified Photodynamical Model for Planetary Mass Determination in Low-Eccentricity Multi-Transiting Systems
论文作者
论文摘要
从运输时机变化中推断行星参数对于小型系外行星来说是挑战，因为它们的过渡可能如此弱，以至于确定单个过境时机是困难或不可能的。我们实现了一个有用的工具组合，共同提供了数字快速的全局光动力学模型。这用于拟合含TTV的灯曲线，以限制低偏心，多个星际系统尤其是小行星，尤其是小行星中的过渡系外行星的质量。我们从开普勒完整的长期数据集中提出了四个多行星系统中推断的动态质量和轨道偏心率。 We test our model against Kepler-36 / KOI-277, a system with some of the most precisely determined planetary masses through TTV inversion methods, and find masses of 5.56 +0.41 -0.45 and 9.76 +0.79 -0.89 m_earth for Kepler-36 b and c, respectively - consistent with literature in both value and error.然后，我们在Kepler -79 / KOI -152中提高了四个行星的质量测定，其中文献值在物理上是有问题的至12.5 +4.5 -3.6，9.5 +2.3 -2：1，11，11，11.3 +2.2 -2.2和6.3 +1.3 +1.0 -1.0 -1.0 -1.0 -1.0 M_EARTH对于Kekpler -79 B，C，C，D和E，相应地相应。我们提供了新的质量约束，而两个系统之前都不存在。这些是开普勒-450 C的12.5 +3.2 -2.6 m_earth，对于Kepler -595 C（以前是KOI -547.03）和B，为3.3 +1.7 -1.0和17.4 +7.1 -3.8 m_earth和B。此处使用的光动力代码称为Pydynamicalc，可公开使用。
Inferring planetary parameters from transit timing variations is challenging for small exoplanets because their transits may be so weak that determination of individual transit timing is difficult or impossible. We implement a useful combination of tools which together provide a numerically fast global photodynamical model. This is used to fit the TTV-bearing light-curve, in order to constrain the masses of transiting exoplanets in low eccentricity, multi-planet systems - and small planets in particular. We present inferred dynamical masses and orbital eccentricities in four multi-planet systems from Kepler's complete long-cadence data set. We test our model against Kepler-36 / KOI-277, a system with some of the most precisely determined planetary masses through TTV inversion methods, and find masses of 5.56 +0.41 -0.45 and 9.76 +0.79 -0.89 m_earth for Kepler-36 b and c, respectively - consistent with literature in both value and error. We then improve the mass determination of the four planets in Kepler-79 / KOI-152, where literature values were physically problematic to 12.5 +4.5 -3.6, 9.5 +2.3 -2:1, 11.3 +2.2 -2.2 and 6.3 +1.0 -1.0 m_earth for Kepler-79 b, c, d and e, respectively. We provide new mass constraints where none existed before for two systems. These are 12.5 +3.2 -2.6 m_earth for Kepler-450 c, and 3.3 +1.7 -1.0 and 17.4 +7.1 -3.8 m_earth for Kepler-595 c (previously KOI-547.03) and b, respectively. The photodynamical code used here, called PyDynamicaLC, is made publicly available.
