标题： 新一代行星种群合成（NGPPS）第八部分。 恒星金属丰度对行星出现率、轨道周期、偏心率和半径山谷形态的影响 显示英文标题

标题： The New Generation Planetary Population Synthesis (NGPPS) VIII. Impact of host star metallicity on planet occurrence rates, orbital periods, eccentricities, and radius valley morphology

摘要： 原行星盘中的尘气比，这可能被刻入宿主恒星的金属丰度，是一个在行星形成过程中起关键作用的特性。 我们旨在通过统计分析由第三代伯尔尼模型生成的行星系统，来限制行星形成和演化过程，并与从观测样本中得出的相关性进行比较。 使用偏向观测完整性的合成行星，我们发现(1)大巨行星和海王星大小的行星的出现率与[Fe/H]正相关，而小型类地行星则表现出负相关。 在两者之间，亚海王星和超级地球的出现率随着[Fe/H]的增加先增加后减少，在0.1 dex处有一个拐点。 (2)轨道周期短于十天的行星更可能围绕金属丰度较高的恒星，这种趋势随着行星半径的增加而减弱。 (3)巨行星和小行星的偏心率与[Fe/H]之间都存在正相关，这可能由外层巨行星的自激发和扰动所解释。 (4)行星半径谷随着[Fe/H]的增加而变得更深且更明显，同时超级地球与亚海王星的比例降低。 此外，谷值以上行星的平均半径随[Fe/H]的增加而增加。 我们的标准模型成功再现了许多与恒星金属丰度相关的观测结果，支持了伯尔尼模型中包含的物理过程和参数的描述。 然而，合成种群预测的轨道偏心率和周期对[Fe/H]的依赖性却显著弱于观测结果。 这种差异表明，行星之间的长期动力学相互作用以及双星/伴星的影响可以将系统推向一个动力学更热的状态。 显示英文摘要

摘要： The dust-to-gas ratio in the protoplanetary disk, which is likely imprinted into the host star metallicity, is a property that plays a crucial role during planet formation. We aim at constraining planet formation and evolution processes by statistically analysing planetary systems generated by the Generation III Bern model, comparing with the correlations derived from observational samples. Using synthetic planets biased to observational completeness, we find that (1) the occurrence rates of large giant planets and Neptune-size planets are positively correlated with [Fe/H], while small sub-Earths exhibit an anti-correlation. In between, for sub-Neptune and super-Earth, the occurrence rate first increases and then decreases with increasing [Fe/H] with an inflection point at 0.1 dex. (2) Planets with orbital periods shorter than ten days are more likely to be found around stars with higher metallicity, and this tendency weakens with increasing planet radius. (3) Both giant planets and small planets exhibit a positive correlation between the eccentricity and [Fe/H], which could be explained by the self-excitation and perturbation of outer giant planets. (4) The radius valley deepens and becomes more prominent with increasing [Fe/H], accompanied by a lower super-Earth-to-sub-Neptune ratio. Furthermore, the average radius of the planets above the valley increases with [Fe/H]. Our nominal model successfully reproduces many observed correlations with stellar metallicity, supporting the description of physical processes and parameters included in the Bern model. However, the dependences of orbital eccentricity and period on [Fe/H] predicted by the synthetic population is however significantly weaker than observed. This discrepancy suggests that long-term dynamical interactions between planets, along with the impact of binaries/companions, can drive the system towards a dynamically hotter state.