Grid-based modelling is widely used for estimating stellar parameters. However, stellar model grid is sparse because of the computational cost. This paper demonstrates an application of a machine-learning algorithm using the Gaussian Process (GP) Regression that turns a sparse model grid onto a continuous function. We train GP models to map five fundamental inputs (mass, equivalent evolutionary phase, initial metallicity, initial helium fraction, and the mixing-length parameter) to observable outputs (effective temperature, surface gravity, radius, surface metallicity, and stellar age). We test the GP predictions for the five outputs using off-grid stellar models and find no obvious systematic offsets, indicating good accuracy in predictions.As a further validation, we apply these GP models to characterise 1,000 fake stars. Inferred masses and ages determined with GP models well recover true values within one standard deviation. An important consequence of using GP-based interpolation is that stellar ages are more precise than those estimated with the original sparse grid because of the full sampling of fundamental inputs.
Pulsational instability of pre-main-sequence models from accreting protostars II. Modelling echelle diagrams of $δ$ Scuti stars without rotational splitting
Modelling $δ$ Scuti pulsations: A new grid of p, g, and f modes across pre-main-sequence to post-main-sequence evolution
Centre for Astrophysics, University of Southern Queensland（南昆士兰大学天体物理中心）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院悉尼天文研究所）
ISOSCELES project: A grid-based quantitative spectroscopic analysis of massive stars
Universidad Mayor（迈约尔大学）；Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso（瓦尔帕莱索大学理学院物理与天文学研究所）；Departamento de Espectroscopía, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球物理科学学院光谱学系）；Instituto de Astrofísica de La Plata, CCT La Plata, CONICET-UNLP（拉普拉塔天体物理研究所，拉普拉塔跨学科研究中心，阿根廷国家科学研究委员会-拉普拉塔国立大学）
An extensive grid of mass fluxes for Galactic O stars
一个先前描述的代码用于构建移动反转层（MRL）的改进，通过替换一个两参数模型的辐射加速由于线与灵活的非参数描述，从而允许更大程度的动力学一致性，以实现在模拟湍流跨音速流在O星的外大气层。用这个新程序计算了（T_eff，g）空间中57个点的质量通量J。具体而言，J是针对所有Lanz-Hubeny（2003）NLTE大气计算的，T_eff（kK）\in（27.5，55）和log g \leq 4.5。与广泛使用的质量损失公式的差异被强调，并确定差分光谱测试的机会。
