两个开普勒红巨星食双星作为红巨星分支下段星震标度关系的基准：来自JKTEBOP和PHOEBE-2建模的动力学质量与半径
Two Kepler red-giant eclipsing binaries as lower red-giant branch benchmarks for asteroseismic scaling relations. Dynamical masses and radii from JKTEBOP and PHOEBE-2 modeling
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中文总结 AI 辅助
本研究利用两个开普勒红巨星食双星KIC 8129189和KIC 10920813，通过JKTEBOP和PHOEBE-2建模获得动力学质量与半径，校准星震标度关系，发现修正因子不依赖半径，支持扩展样本以验证标度关系。
中文摘要 AI 辅助
空间光度测量已在数千颗恒星中探测到类太阳振荡，其全局地震参数通过星震标度关系给出恒星性质。由于这些关系系统性地高估红巨星的质量和半径，因此需要经验校准。包含振荡红巨星的双线食双星无需外部校准即可提供精确的动力学质量和半径，使其成为理想的基准。我们展示了KIC 8129189和KIC 10920813，这两个包含演化程度较低的振荡红巨星的Kepler食双星，作为将校准样本扩展到更小半径的新基准。我们从高分辨率光谱测量了视向速度，从Kepler光变曲线提取了全局星震参数，并使用JKTEBOP和PHOEBE-2对双星进行了建模，采用了完整光变曲线和选定的食组，从测试的模型/数据配置包络中采用了基准质量和半径。然后我们将修正因子$f_{\Delta\nu}$和$f_{\nu_{max}}$拟合到基础的$\Delta\nu$-密度和$\nu_{max}$-表面重力关系。我们得到KIC 8129189的$M_{RG}=1.413 \pm 0.037 M_\odot$和$R_{RG}=4.296 \pm 0.061 R_\odot$，以及KIC 10920813的$M_{RG}=1.383 \pm 0.022 M_\odot$和$R_{RG}=5.914 \pm 0.043 R_\odot$。采用的15星校准给出$f_{\Delta\nu}=0.9777 \pm 0.0048$和$f_{\nu_{max}}=1.024 \pm 0.008$，对应于$C_M=0.850 \pm 0.020$和$C_R=0.9333 \pm 0.0090$。两个修正因子均不显著依赖于半径，$f_{\nu_{max}}$也不依赖于金属丰度；基于模型的$f_{\Delta\nu}$值系统性地低于动力学推导值。两个系统与先前基准的修正一致，表明继续扩展食双星样本对于跨演化阶段测试标度关系至关重要。
英文摘要
Space-based photometry has detected solar-like oscillations in thousands of stars, whose global seismic parameters yield stellar properties via the asteroseismic scaling relations. Because these relations systematically overestimate red-giant masses and radii empirical calibration is required. Double-lined eclipsing binaries hosting oscillating red giants provide precise dynamical masses and radii without external calibration, making them ideal benchmarks. We present KIC 8129189 and KIC 10920813, two Kepler eclipsing binaries containing less-evolved oscillating red giants, as new benchmarks that extend the calibration sample toward smaller radii. We measured radial velocities from high-resolution spectra, extracted global asteroseismic parameters from Kepler light curves, and modeled the binaries with JKTEBOP and PHOEBE-2 using both full light curves and selected eclipse sets, adopting benchmark masses and radii from the envelope of tested model/data configurations. We then fit correction factors $f_{Δν}$ and $f_{ν_{max}}$ to the underlying $Δν$-density and $ν_{max}$-surface-gravity relations. We obtain $M_{RG}=1.413 \pm 0.037 M_\odot$ and $R_{RG}=4.296 \pm 0.061 R_\odot$ for KIC 8129189, and $M_{RG}=1.383 \pm 0.022 M_\odot$ and $R_{RG}=5.914 \pm 0.043 R_\odot$ for KIC 10920813. The adopted 15-star calibration gives $f_{Δν}=0.9777 \pm 0.0048$ and $f_{ν_{max}}=1.024 \pm 0.008$, corresponding to $C_M=0.850 \pm 0.020$ and $C_R=0.9333 \pm 0.0090$. Neither correction factor depends significantly on radius, nor does $f_{ν_{max}}$ depend on metallicity; model-based $f_{Δν}$ values are systematically lower than the dynamically derived ones. Both systems agree with the correction from previous benchmarks, showing that continued expansion of the eclipsing-binary sample is essential for testing the scaling relations across evolutionary stage.
发表机构
- Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）
- Thüringer Landessternwarte（图林根州天文台）
- Department of Astronomy, New Mexico State University（新墨西哥州立大学天文学系）
- Institut d’Astrophysique Spatiale, UMR 8617, Université Paris-Saclay, CNRS（巴黎萨克雷大学CNRS空间天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。
