基于MESA模型的亚巨星质量与半径新标度关系：开普勒目标星的应用
New scaling relations from MESA models for mass and radius of subgiant stars: application to Kepler targets
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中文总结 AI 辅助
该研究基于MESA模型构建亚巨星质量与半径的新标度关系，应用于31颗开普勒观测的亚巨星，提升了恒星质量与半径的测定精度，为星震学分析提供了新工具。
中文摘要 AI 辅助
精确测定恒星基本参数对理解恒星结构与演化至关重要。在这方面，空间望远镜获取的类太阳振荡恒星的星震学参数，可结合经典标度关系测定单星的质量（$M$）与半径（$R$），但这些标度关系仍需改进。本研究针对亚巨星（SG），基于氦电离区 glitch 产生的参考频率（$\nu_{\rm min}$）构建替代标度关系。我们汇编文献中的主序星与亚巨星MESA模型，推导演化恒星的$R$与表面重力（$g$）的新标度关系，$R$与$g$的表达式同时作为大频率间隔、$\nu_{\rm min}$与金属丰度的函数。这些新关系仅通过观测参数即可可靠测定$M$与$R$，无需详细恒星建模。将基于$\nu_{\rm min}$的新关系应用于开普勒（Kepler）任务观测的31颗亚巨星样本，这些恒星质量范围为0.85-1.74 M$_\bigodot$，半径范围为1.03-2.82 R$_\bigodot$。通过联立求解，我们估算出这些恒星新的质量范围为0.89-1.62 M$_\bigodot$，半径范围为1.04-2.95 R$_\bigodot$。结果表明，新关系显著提升了对开普勒目标演化恒星的$M$与$R$的测定精度，凸显了其在星震学分析中的应用潜力。
英文摘要
The precise determination of the fundamental parameters of stars is crucial for understanding stellar structure and evolution. In this regard, the asteroseismic parameters of solar-like oscillating stars obtained from space telescopes are very useful for determining the mass ($M$) and radius ($R$) of single stars using classical scaling relations. These relations still need to be improved. In this study, we develop alternative scaling relations based on reference frequencies ($ν_{\rm min}$) due to helium ionization zone glitches, specifically for subgiant (SG) stars. We compile main-sequence and SG {\small{MESA}} models from the literature and derive new scaling relations for stellar $R$ and surface gravity ($g$) of evolved stars. The expressions for $R$ and $g$ are obtained simultaneously as functions of the large frequency separation, $ν_{\rm min}$, and metallicity. These new relations allow $M$ and $R$ to be reliably determined only from observational parameters, without the need for detailed stellar modelling. The resulting $ν_{\rm min}$-based relations are applied to a sample of 31 SG stars observed by the \emph{Kepler} mission, with masses in the range 0.85-1.74 M$_\odot$ and radii between 1.03 and 2.82 R$_\odot$. Using simultaneous solutions, we estimate new mass and radius ranges of 0.89-1.62 M$_\odot$ and 1.04-2.95 R$_\odot$, respectively. The results demonstrate significant improvements in the determination of $M$ and $R$ for evolved \emph{Kepler} target stars, highlighting the potential of the new scaling relations in asteroseismic analyses.
发表机构
- Ege University（伊兹密尔伊ege大学）
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