AI 中文总结
本研究开发了与MESA集成的Custom Colors模块（含Python包SED_Model），可在恒星演化计算中实时将恒星模型转换为合成测光，通过六个用例验证，其中两项与观测数据比对精度达1.1%周期、0.2%振幅。
AI 中文摘要
恒星演化模拟会预测光度等物理量，而宽带测光观测则测量特定通带内的流量；将预测的恒星状态转换为星等需要在表面参数处插值恒星大气模型，将得到的光谱能量分布（SED）与滤光片透射曲线卷积，并应用测光零点校正。我们引入Custom Colors，该模块可完成从恒星模型到上述测光量的转换。它作为MESA Custom Colors集成到MESA中，同时以Python包SED_Model的形式提供给外部应用。在每个时间步，该模块会在当前有效温度T_eff、表面重力log g、金属丰度[M/H]处插值用户指定的大气网格，应用用户指定距离下的几何稀释，将SED与每个请求的滤光片透射曲线卷积，并将观测框架星等附加到标准MESA输出文件中。我们在六种不同的用例中演示了该模块：TP-AGB演化、非线性天琴座RR型变星脉动、星斑修正的光球、白矮星冷却、蓝环演化，以及基于外部YREC SPOTS网格的旋转星斑调制。这些用例使用了Kurucz/ATLAS9、BT-Settl和Koester DA大气网格，以及Roman WFI、LSST ugrizy、Gaia和扩展Johnson UBVRIJHKLMN滤光系统。其中两项演示直接将该模块与观测数据进行了比较：一个0.6M☉的DA白矮星冷却轨迹遵循Gaia DR3的宽冷却轨迹，从M_G≈8.5到15mag，无需中间颜色转换；一个RSP模型恢复了天琴座FN（KIC6936115）的开普勒光变曲线，周期精度达1.1%，振幅精度达0.2%。
英文摘要
Stellar evolution simulations predict physical quantities such as luminosity, whereas broadband photometric observations measure flux in specific bandpasses; converting the predicted stellar state to magnitudes requires interpolating a stellar atmosphere model at the surface parameters, convolving the resulting spectral energy distribution (SED) with filter transmission curves, and applying a photometric zero-point correction. We introduce Custom Colors, which performs this conversion from the stellar model. It is integrated into MESA as MESA Custom Colors, and available as the Python package SED_Model for external applications. At each timestep, the module interpolates a user-specified atmosphere grid at the current T_eff, log g, [M/H], applies geometric dilution at a user-specified distance, convolves the SED with each requested filter transmission curve, and appends observer-frame magnitudes to standard MESA output files. We demonstrate the module across six diverse use cases: TP-AGB evolution, nonlinear RR Lyrae pulsation, starspot-modified photospheres, white dwarf cooling, blue-loop evolution, and rotational spot modulation based on an external YREC SPOTS grid. These cases draw on Kurucz/ATLAS9, BT-Settl, and Koester DA atmosphere grids and filter systems including Roman WFI, LSST ugrizy, Gaia, and extended Johnson UBVRIJHKLMN. Two of these demonstrations compare the module directly with observational data: a 0.6M_dot DA white dwarf cooling track follows the broad Gaia DR3 cooling locus from M_G ~ 8.5 to 15mag without intermediate color transformation, and an RSP model recovers the Kepler light curve of FN Lyr (KIC6936115) to 1.1% in period and 0.2% in amplitude.
Comments24 pages, 15 figures. Submitted to ApJ. Feedback welcome
