Exploring the Diversity of Exoplanets Bulk Densities in multi-parameter space

该项目由位于德国柏林-阿德尔肖夫中心(DLR-EPA)、Thüringer Landessternwarte Tautenburg(TLS)和科隆大学莱茵研究所(RIU-PF)的三个密切合作的德国团队提出，他们在恒星光曲线(RIU，DLR)、径向速度测量和解释(TLS)和凌日模型(DLR)的凌日探测方面拥有丰富的经验。与社区中的其他努力不同，所有这些专门知识都在一个工作组中得到维护。这一提议旨在了解行星密度中发现的结构作为几个行星参数(质量、标度距离、日照强度等)的函数，旨在发现更多感兴趣的质量范围内的行星，它可以提供关于系外行星形成和演化的线索，因此将对SPP提出的基本问题作出重大贡献。这一建议还与我们自己的观测和研究在SPP第一阶段提出的问题相联系：(1)精确和一致地重新计算以测量质量为基础的行星系的恒星、行星和轨道性质，以实现这些目标；(2)了解低质量(3-11摩尔)和中等(11-100摩尔)质量行星在质量-密度图中的分布。第三个参数(日照度、刻度半长轴等)能否帮助解释分布？；(Iii)从质量密度图和行星探测了解低质量行星和巨行星之间的冰行星是如何形成的；(Iv)考虑到巨行星和棕矮星的性质(质量密度关系、形成方式、内部结构等)，定义巨行星和棕矮星之间的边界；(V)更准确地定义棕矮星和新发现的恒星之间的过渡质量；(Vi)研究超短周期行星：潮汐下的生存预期和蒸发质量损失，形状变形，可能为其形成提供线索。之前的资助期间使我们能够完成我们的K2活动，并专注于对Tess过境考生的研究。在下一个资助期内，我们希望继续对Tess和Cheops光曲线进行科学开发。这项工作还将使该联盟和德国社区为柏拉图时代的系外行星科学做好准备。

This project is proposed by a consortium of three closely working German teams located at DLR Berlin-Adlershof (DLR-EPA), the Thüringer Landessternwarte Tautenburg (TLS) and the Rheinisches Institut für Umweltforschung at the University Cologne in Köln (RIU-PF) who have a considerable experience in transit detection in stellar light curves (RIU, DLR), in radial velocity measurements and interpretation (TLS) and in transit modelling (DLR). Unlike other efforts in the community all of this expertise is maintained in a single working group. This proposal aims at understanding the structures found in the planet densities as a function of several planetary parameters (mass, scaled distance, insolation, etc.), aims at discovering many more planets in the mass range of interest and that it can provide clues as to the formation and evolution of exoplanets and will therefore make a substantial contribution to the fundamental question posed by SPP. This proposal also connects to questions raised during the first phase of SPP from our own observations and research: (i) recompute precisely and consistently the stellar, planetary and orbital properties of planetary systems with measured mass as a base to achieve the objectives; (ii) understand the distribution of the low (3-11 Mearth) and intermediate (11-100 Mearth) mass planets in the mass-density diagram. Can a third parameter (insolation, scaled semi-major axis etc) help to explain the distribution?; (iii) understand from the mass-density diagram and planet detections how the ice planets between low mass planets and giant planets form; (iv) define the boundary between giant planets and Brown Dwarfs considering their properties (mass-density relationship, formation, interiors etc.); (v) Define more precisely the transition mass between Brown Dwarfs and stars from new discoveries; (vi) study ultra-short period planets: survival expectancy under tides, and mass loss by evaporation, shape deformations which may give clues on their formation. The previous funding period enabled us to complete our K2 activities and to focus on the study of TESS transit candidates. During the next funding period we want to proceed with the science exploitation of TESS and CHEOPS light curves. This work will also prepare this consortium and the German community for exoplanet science in the PLATO era.