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

这个项目是由三个紧密合作的德国团队组成的财团提出的，他们分别位于柏林-阿德勒绍夫DLR （DLR- epa）、th<s:1> ringer Landessternwarte Tautenburg （TLS）和德国科隆大学Köln （RIU- pf）的Rheinisches研究所<s:2> Umweltforschung (RIU， DLR)，他们在恒星光曲线的凌日探测（RIU， DLR）、径向速度测量和解释（TLS）和凌日建模（DLR）方面拥有丰富的经验。与社区中的其他工作不同，所有这些专业知识都由一个工作组维护。这个提议的目的是理解在行星密度中发现的结构作为几个行星参数（质量、比例距离、日晒等）的函数，旨在发现更多的系外行星，它可以为系外行星的形成和演化提供线索，因此将对SPP提出的基本问题做出重大贡献。这一建议也与SPP第一阶段提出的问题联系起来，这些问题来自我们自己的观察和研究：(i)以测量质量为基础，精确和一致地重新计算行星系统的恒星、行星和轨道特性，以实现目标；（ii）了解质量密度图中低质量（3-11地球质量）和中等质量（11-100地球质量）行星的分布。第三个参数（日照、缩放半长轴等）是否有助于解释分布？（iii）从质量密度图和行星探测中了解低质量行星和巨大行星之间的冰行星是如何形成的；（iv）根据巨行星和褐矮星的性质（质量密度关系、形成、内部等）定义它们之间的界限；(v)更精确地定义新发现的褐矮星和恒星之间的过渡质量；（六）研究超短周期行星：潮汐作用下的生存预期、蒸发造成的质量损失、形状变形，这些可能为它们的形成提供线索。之前的资助期使我们能够完成K2活动，并专注于TESS过境候选者的研究。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。这项工作也将使该联盟和德国社区为PLATO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.