PySeshat：用于双星轨道确定和Al-Wardat恒星大气建模的经过验证的Python流水线
PySeshat: A Validated Python Pipeline for Binary-Star Orbit Determination and Al-Wardat Stellar Atmosphere Modeling
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中文总结 AI 辅助
PySeshat是一个开源Python流水线，统一双星与层级三星轨道确定和恒星SED拟合，经十二个真实基准系统验证，支持同时拟合内外轨道，解决近等温组分温度简并问题。
中文摘要 AI 辅助
精确的恒星质量以及双星和多星系统的物理参数分别需要约束良好的轨道解和独立的恒星大气建模。现有的开源软件分别处理这些问题，而层级三星系统额外需要同时拟合其内轨道和外轨道，现有工具中很少有提供这种处理。我们介绍了PySeshat，一个开源的Python包，将双星和层级三星轨道确定与恒星SED拟合统一在单一、经过验证的流水线中。该包通过最小二乘法拟合目视、光谱和组合双星轨道，并通过两种并行形式拟合层级三星轨道，其中一种形式同时拟合内轨道和外轨道，而不是顺序拟合。两者共享一个共同的贝叶斯后验采样层。第二个模块将双组分合成光谱拟合到双星组合的、未分辨的光度测量中，以恢复每个组分的温度和半径。该软件针对十二个真实的、已发表的基准系统进行了验证，并与三个独立的轨道拟合包以及真实的太空望远镜档案数据进行了交叉检查。所有十二个基准系统达到的拟合质量与其已发表的解一致。在相同的真实系统上比较同时和顺序三星拟合形式表明，同时方法不仅是可取的，而且是必要的：一个系统的轨道配置根本无法由顺序形式表示。拟合四个独立发表的系统的光度测量揭示了在从未分辨的光中恢复近双胞胎温度恒星组分的单个温度时存在简并性，这与可用的光度数据量无关。该包为双星和多星系统分析提供了一个经过验证的、开放的和可扩展的流水线，已公开发布并可自由安装。
英文摘要
Precise stellar masses and physical parameters for binary and multiple star systems require, respectively, well-constrained orbital solutions and independent stellar-atmosphere modeling. Existing open-source software addresses these separately, and hierarchical triple systems additionally require simultaneous fitting of their inner and outer orbits, a treatment few existing tools provide. We present PySeshat, an open-source Python package unifying binary and hierarchical-triple orbit determination with stellar SED fitting in a single, validated pipeline. The package fits visual, spectroscopic, and combined binary orbits by least-squares, and hierarchical-triple orbits through two parallel formalisms, one of which fits both inner and outer orbits simultaneously rather than sequentially. Both share a common Bayesian posterior-sampling layer. A second module fits two-component synthetic spectra to a binary's combined, unresolved photometry to recover each component's temperature and radius. The software was validated against twelve real, published benchmark systems, cross-checked against three independent orbit-fitting packages and real space-telescope archive data. All twelve benchmark systems reach fit quality consistent with their published solutions. Comparing the simultaneous and sequential triple-fitting formalisms on the same real systems shows the simultaneous approach is not merely preferable but necessary: one system's orbital configuration cannot be represented by the sequential formalism at all. Fitting four independently published systems' photometry reveals a degeneracy in recovering individual temperatures for near-twin-temperature stellar components from unresolved light, independent of how much photometric data is available. The package provides a validated, open, and extensible pipeline for binary and multiple star system analysis, publicly released and freely installable.
发表机构
- Faculty of Science, Cairo University（开罗大学理学院）
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