AI 中文总结
本研究系统探究含金属丰度和自转效应的γ Doradus 星理论不稳定带，构建大型模型网格，其结果与观测吻合良好，相关网格已公开。
AI 中文摘要
开普勒等近期空间任务提供了γ Doradus 不稳定带（IS）的大规模观测数据，可用于约束模型并探索其局限性，其中一个长期存在的局限性是γ Doradus IS 蓝边的预测，观测到大量γ Doradus 星分布在该区域。尽管观测取得进展，但尚未开展系统研究以探究不同物理过程对γ Doradus IS 的影响。本研究旨在利用现代工具系统探究理论γ Doradus IS，考虑金属丰度和自转的效应，为科学界提供大型模型网格及其振荡参数。我们研究了恒星模型网格的非绝热脉动性质，模型质量范围为1.35 M☉至2.5 M☉，金属丰度Z=0.01至Z=0.025，刚体自转速率范围为Ω=0至0.5 Ωcrit（Ωcrit为临界自转速率）。结果表明，所有计算中，理论γ Doradus IS 与观测IS 吻合良好，仅在延伸的蓝色区域存在差异；在径向阶数方面，我们的模型一致重现了l=1、l=2 和罗斯比模的激发模式，与观测结果大致吻合，且激发径向阶数的范围强烈依赖于有效温度。激发径向阶数的范围可用于约束恒星在γ Doradus IS 内的位置，或为解释蓝色区域观测到的差异的物理机制提供线索。所有计算的模型网格均已公开，包含γ Doradus 星的模式阻尼和增长率，通过对流-振荡相互作用的时变处理获得。
英文摘要
Recent space missions such as Kepler have provided large-scale observations of the γ-Doradus instability strips (IS), which can be used to constrain models and explore their limitations. One persistent limitation is the prediction of the blue edge of the γ- Doradus IS, where a significant number of γ-Doradus stars are observed. Despite these observational advances, no systematic study has been undertaken to explore the effects of different physical processes on the γ-Doradus. Our aim is to systematically explore the theoretical γ-Doradus IS with modern tools, accounting for the effects of rotation and metallicity, providing a large grid of models and their oscillation parameters for the scientific community. We investigated the non-adiabatic pulsation properties of stars in a grid of stellar models with masses between 1.35 M{_\odot} and 2.5 M{_\odot}, metallicities between Z= 0.01 and Z= 0.025, and solid-body rotation rates ranging from Ω = 0 to 0.5 {Ω_{crit}}, where {Ω_{crit}} denotes the critical rotation rate. We find that, across all computations, the theoretical γ-Doradus IS agrees well with the observed IS, except in the extended blue region. In terms of radial orders, our models consistently reproduce the excited modes in broad agreement with observations for l= 1, l= 2, and Rossby modes. We also show that the range of excited radial orders is strongly dependent on the effective temperature. The range of excited radial orders can be used to constrain the position of a star within the γ-Doradus IS and may provide insights into the physical mechanisms responsible for the discrepancies observed in the blue region. All computed grids are made available and include mode damping and growth rates for γ-Doradus stars, obtained with a time-dependent treatment of the convection-oscillation interaction.
Commentsaccepted for publication in A&A
