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arXiv 2107.09205astro-ph.SR
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巨星有效温度和线半径的直接测量：光谱类型和V-K颜色的定标

Direct Measurements of Giant Star Effective Temperatures and Linear Radii: Calibration Against Spectral Types and V-K Color

Gerard T. van Belle, Kaspar von Braun, David R. Ciardi, Genady Pilyavsky, Ryan S. Buckingham, Andrew F. Boden, Catherine A. Clark, Zachary Hartman, Gerald van B… 展开作者

Gerard T. van Belle, Kaspar von Braun, David R. Ciardi, Genady Pilyavsky, Ryan S. Buckingham, Andrew F. Boden, Catherine A. Clark, Zachary Hartman, Gerald van Belle, William Bucknew, Gary Cole

备注：
310 pages, 16 figures, 21 tables, accepted to be published in The Astrophysical Journal
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摘要：

我们计算直接确定的有效温度（$T_{\rm EFF}$）和半径（$R$）的191巨星的高分辨率角尺寸测量的基础上，从光学干涉在帕洛玛试验台干涉仪。巨星的窄波段到宽波段测光数据被用来通过光谱能量分布拟合建立热辐射通量和光度，这允许均匀地建立光谱类型和去红$V_{\rm 0}-K_{\rm 0}$颜色的评估;这两个参数被用作建立$T_{\rm EFF}$和$R$趋势的校准指数。光谱类型范围从G 0 III到M7.75 III，$V_{\rm 0}-K_{\rm 0}$从1.9到8.5。对于$V_{\rm 0}-K_{\rm 0} = \{1.9,6.5\}$范围，中值$T_{\rm EFF}$不确定性的有效温度与颜色的拟合被发现小于50 K;在这个范围内，$T_{\rm EFF}$从5050 K下降到3225 K。发现从G 0 III到K 0 III，线性大小在11 $R_\odot$处基本恒定，随着亚型线性增加，在K5 III处增加到50 $R_\odot$，然后通过M8 III进一步线性增加到150 $R_\odot$。该数据集的效用的三个例子：第一，一个完全经验的赫兹-罗素图构造和检查恒星演化模型;第二，恒星质量的值推断的基础上的措施$R$和文献值为$\log g$。最后，提出了一种基于恒星的$V$和$K$值的角尺寸预测工具的改进校准。

英文摘要：

We calculate directly determined values for effective temperature ($T_{\rm EFF}$) and radius ($R$) for 191 giant stars based upon high resolution angular size measurements from optical interferometry at the Palomar Testbed Interferometer. Narrow- to wide-band photometry data for the giants are used to establish bolometric fluxes and luminosities through spectral energy distribution fitting, which allow for homogeneously establishing an assessment of spectral type and dereddened $V_{\rm 0}-K_{\rm 0}$ color; these two parameters are used as calibration indices for establishing trends in $T_{\rm EFF}$ and $R$. Spectral types range from G0III to M7.75III, $V_{\rm 0}-K_{\rm 0}$ from 1.9 to 8.5. For the $V_{\rm 0}-K_{\rm 0} = \{1.9,6.5\}$ range, median $T_{\rm EFF}$ uncertainties in the fit of effective temperature versus color are found to be less than 50K; over this range, $T_{\rm EFF}$ drops from 5050K to 3225K. Linear sizes are found to be largely constant at 11 $R_\odot$ from G0III to K0III, increasing linearly with subtype to 50 $R_\odot$ at K5III, and then further increasing linearly to 150 $R_\odot$ by M8III. Three examples of the utility of this data set are presented: first, a fully empirical Hertzsprung-Russell Diagram is constructed and examined against stellar evolution models; second, values for stellar mass are inferred based on measures of $R$ and literature values for $\log g$. Finally, an improved calibration of an angular size prediction tool, based upon $V$ and $K$ values for a star, is presented.

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