论文标题
HD3167系统的Cheops增强视图
A CHEOPS-enhanced view of the HD3167 system
论文作者
论文摘要
关于超过海王星的系外行星的性质还有很多待理解，其中大多数是在紧凑的多个星际系统中发现的。由于其内部超短期行星B与恒星和两个较大的外行星D-C在极轨道上对齐，因此多星际系统HD 3167具有特殊的结构，并提供了研究动态和大气进化过程的可能性。为此，我们结合了多个传输光度法和径向速度法（RV）的多个数据集，以修改系统的属性并告知其行星模型。 HD 3167B的Cheops观察结果使这项努力带头，尽管它极端辐照，但似乎与纯粹的岩石成分不一致。 Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial气态信封。我们在较大的轨道上检测到第四个，更大的行星，可能具有HD 3167D-C的共面。动态模拟确实表明，在系统历史的早期，当HD 3167b仍然受到恒星影响并保持其对齐的轨道时，整个行星系统d-c-e在系统历史的早期就被倾斜了。 RV数据和直接成像规则规定，可能负责当前体系结构的同伴仍绑定到HD \ 3167系统。类似的全球多样品系统研究将证明有多少共享HD3167系统的特性，该系统仍然是随访观测和模拟的首选目标。
Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD\,3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD3167 system, which remains a target of choice for follow-up observations and simulations.
