发表机构
STAR Institute, Université de Liège; Department of Physics and Astronomy, Uppsala University; Institut für Astrophysik, Zürich Universität; Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM; Instituto de Astrofísica de Canarias (IAC); Universidad de La Laguna (ULL), Departamento de Astrofísica（列日大学 STAR 研究所; 乌普萨拉大学物理与天文学系; 苏黎世大学天体物理研究所; 巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学与信息分子实验室; 加那利群岛天体物理研究所; 拉古纳大学天体物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究针对六个Kepler/K2太阳模拟体，评估物理输入（如不透明度、核反应速率）对恒星参数确定的影响，发现质量恢复精度达2.5%，年龄系统误差多为10-14%，部分情况低于4%，满足PLATO任务精度要求。
AI 中文摘要
太阳模拟体是测试恒星结构和演化的有用实验室，特别是在即将到来的PLATO任务的背景下。我们的研究聚焦于由Kepler和K2观测到的六个地震太阳模拟体。我们调查了模型物理成分对这六个目标的影响，以评估在当前可用的数据质量下，我们能在多大程度上满足PLATO对恒星参数的精度要求。我们使用通过正向和反向组合（FICO）程序获得的恒星质量、年龄和化学组成作为参考值，该程序基于OPAL不透明度以及NACRE II和Solar Fusion II（SFII）核反应速率的组合。宏观输运的效率根据从HERMES光谱分析得出的锂丰度进行校准。在此基础上，我们借助Levenberg-Marquardt局部最小化方法，利用经典和地震约束对物理成分进行了广泛测试。特别地，我们调查了使用OPLIB不透明度和SFIII核反应速率对恒星基本性质的影响，以及使用各种地震约束的影响。我们量化了建模输入物理变化可能导致的潜在差异，并将其程度与PLATO任务预期要求（质量15%、半径2%、年龄10%）进行比较，为PLATO确定基本性质的准确性和鲁棒性（相对于系统误差）提供了关键约束。对于我们的太阳模拟体样本，我们能够在2.5%以内准确恢复恒星质量。至于恒星年龄，我们量化了最多约10-14%的系统误差，但也有非常有希望的情况，根据所考虑的恒星和约束，偏差保持在4%以内。
英文摘要
Solar analogs are useful laboratories for tests of stellar structure and evolution, particularly in the context of the upcoming PLATO mission. Our study focuses on six seismic solar analogs observed by Kepler and K2. We investigate the impact of the model physical ingredients on these six targets in order to evaluate how well one can satisfy the PLATO precision requirements for stellar parameters with the data quality that is currently available to us. We used as reference values the stellar mass, age, and chemical composition obtained with the Forward and Inverse COmbination (FICO) procedure, based on OPAL opacities and a combination of NACRE II and Solar Fusion II (SFII) nuclear reaction rates. The efficiency of macroscopic transport is calibrated on lithium abundances derived from the analysis of HERMES spectra. From there, we carried out extensive tests of the physical ingredients with the help of a Levenberg-Marquardt local minimisation method using both classical and seismic constraints. In particular, we investigated the impact induced by the use of OPLIB opacities and SFIII nuclear reaction rates on the stellar fundamental properties, as well as the use of various seismic constraints. We quantify the potential differences that changes in the modelling input physics may lead to, and compare their extent with the requirements expected for the PLATO mission (15% in mass, 2% in radius, and 10% in age), providing crucial constraints on the accuracy and robustness with respect to systematics of the determination of fundamental properties for PLATO. For our sample of solar analogs, we are able to accurately retrieve stellar masses within 2.5%. As for stellar ages, we quantify systematics of the order of 10-14% at most, but there are also very promising cases for which deviations remain within 4% depending on the stars and constraints considered.
Comments11 pages, 10 figures, accepted for publication in A&A (shortened abstract)
