Orbital obliquity sampling in the Kepler-20 system using the 3D animation software Blender
Orbital obliquity sampling in the Kepler-20 system using the 3D animation software Blender
复制标题
使用 3D 动画软件 Blender 在 Kepler-20 系统中进行轨道倾斜采样
DOI：
10.1051/0004-6361/202141627
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发表时间：
2022
影响因子：
6.5
通讯作者：
J.H.M.M.
中科院分区：
文献类型：
--
作者：
Müller;Ioannidis;Schmitt;J.H.M.M.
多行星系统中的相互轨道对齐是理解其形成的重要参数。有许多精细的技术来使用光度或光谱数据确定对准参数。行星-行星掩星（PPO），可能发生在多个凌日系统中，就是一个直观的例子。虽然存在的PPO约束的轨道排列，没有乍一看doesn 't.AimsPlanetary系统，其中的测量的轨道平行度与传统的技术仍然难以捉摸，要求新的方法，至少可以获得一些信息的路线。在这里，我们开发了一种方法，使用光度数据，以获得这种信息从多凌events.MethodsIn我们的方法，我们合成多过境光变曲线的系外行星的问题，通过构建一个网格的投影轨道倾角α，同时保持所有的过境参数恒定。这些模型光变曲线包含某些α值的PPO。为了计算模型光变曲线，我们使用3D动画软件Blender进行凌日模拟，它允许使用星星的任意表面亮度分布，例如模型大气的临边变暗。由此产生的模型光变曲线，然后比较实际measurement.ResultsWe提出了一个详细的研究多凌日行星系统开普勒-20，包括参数拟合的凌日行星和恒星活动的分析。我们将我们的方法应用于Kepler-20 B和C，在那里我们能够排除一些轨道几何形状，并发现这些行星在不同恒星半球前方以顺行方向日食的趋势。结论尽管我们的结果在Kepler-20的情况下统计显着性较低，但我们认为我们的方法对于PPO信号大于噪音的系统很有价值。根据我们的分析，对于像开普勒-20 B这样的行星，噪声≤ 2 × 10− 4，或者对于较小的分量和像开普勒-20一样的测光，行星半径≥ 3 RE，就足以获得重要的结果。
ContextThe mutual orbital alignment in multiple planetary systems is an important parameter for understanding their formation. There are a number of elaborate techniques to determine the alignment parameters using photometric or spectroscopic data. Planet–planet occultations (PPOs), which can occur in multiple transiting systems, are one intuitive example. While the presence of PPOs constrains the orbital alignment, the absence at first glance does not.AimsPlanetary systems, for which the measurement of orbital obliquities with conventional techniques remains elusive, call for new methods whereby at least some information on the alignments can be obtained. Here we develop a method that uses photometric data to gain this kind of information from multi-transit events.MethodsIn our approach we synthesize multi-transit light curves of the exoplanets in question via the construction of a grid of projected orbital tilt anglesα, while keeping all transit parameters constant. These model light curves contain PPOs for some values ofα. To compute the model light curves, we use the 3D animation software Blender for our transit simulations, which allows the use of arbitrary surface brightness distributions of the star, such as limb darkening from model atmospheres. The resulting model light curves are then compared to actual measurements.ResultsWe present a detailed study of the multi-transiting planetary system Kepler-20, including parameter fits of the transiting planets and an analysis of the stellar activity. We apply our method to Kepler-20 b and c, where we are able to exclude some orbital geometries, and find a tendency of these planets to eclipse in front of different stellar hemispheres in a prograde direction.ConclusionsDespite the low statistical significance of our results in the case of Kepler-20, we argue that our method is valuable for systems where PPO signals larger than the noise can occur. According to our analysis, noise ≤ 2 × 10−4for planets like Kepler-20 b, or a planet radius ≥ 3REarthfor the smaller component and Kepler-20-like photometry, would be sufficient to achieve significant results.