论文标题
斑点模型：理论恒星进化轨道和等质线的网格，用于测试星形对结构和颜色的影响
The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors
论文作者
论文摘要
一维恒星进化模型已成功地代表了各种天体物理环境中恒星的结构和演变，但是在年轻的，磁性的恒星以及具有潮汐相互作用显着的近距离二元恒星的背景下，并发症已引起并发症。许多拼图与智前序列和活跃的主序列恒星有关，与它们的半径，其颜色，某些元素丰度和年轻簇的同时性有关。这些难题的一个有希望的解释是磁性活性和星形对活性恒星结构的扭曲作用。为了帮助社区评估这一假设，我们介绍了带有星形（斑点）模型的轨道的恒星参数，太阳金属性恒星进化轨道和等距离的网格，其中包括恒星点的结构效应。这些模型范围为0.1-1.3 \ msun，从点覆盖为85 \％的表面范围，并且从前序列序列演变为红色巨型分支（或15 〜Gyr）。我们还使用经验校准的彩色表为模型生成了两倍的合成色。我们描述了斑点模型中包含的物理成分，并将其预测与其他现代进化代码进行了比较。最后，我们将这些模型应用于活跃恒星领域的几个开放问题，包括年轻的黯然失色的二进制室的半径，前序列序列恒星的颜色尺度以及亚毛的存在，表明我们的模型可以解释许多活跃恒星的许多特征。
One-dimensional stellar evolution models have been successful at representing the structure and evolution of stars in diverse astrophysical contexts, but complications have been noted in the context of young, magnetically active stars, as well as close binary stars with significant tidal interactions. Numerous puzzles are associated with pre-main sequence and active main-sequence stars, relating to their radii, their colors, certain elemental abundances, and the coevality of young clusters, among others. A promising explanation for these puzzles is the distorting effects of magnetic activity and starspots on the structure of active stars. To assist the community in evaluating this hypothesis, we present the Stellar Parameters Of Tracks with Starspots (SPOTS) models, a grid of solar-metallicity stellar evolutionary tracks and isochrones which include a treatment of the structural effects of starspots. The models range from 0.1-1.3\msun and from spot-less to a surface covering fraction of 85\%, and are evolved from the pre-main sequence to the red giant branch (or 15~Gyr). We also produce two-temperature synthetic colors for our models using empirically-calibrated color tables. We describe the physical ingredients included in the SPOTS models and compare their predictions to other modern evolution codes. Finally, we apply these models to several open questions in the field of active stars, including the radii of young eclipsing binaries, the color scale of pre-main sequence stars, and the existence of sub-subgiants, demonstrating that our models can explain many peculiar features of active stars.
