arXivDaily arXiv每日学术速递 周一至周五更新
北美退伍军人节（Veterans Day），12 日无更新
arXiv 1801.03570astro-ph.SR
收藏

HAT-TR-318-007：由HATNet发现并由K2观测的双线M矮星双星，具有总的次级食

HAT-TR-318-007: a double-lined M-dwarf binary with total secondary eclipses discovered by HATNet and observed by K2

J. D. Hartman, S. N. Quinn, G. Á. Bakos, G. Torres, G. Kovács, D. W. Latham, R. W. Noyes, A. Shporer, B. J. Fulton, G. A. Esquerdo, M. E. Everett, K. Penev, W. Bhatti, Z. Csubry

备注：
34 pages, 22 figures, 15 tables, accepted for publication in AJ
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

我们报告了HAT-TR-318-007的HATNet巡天发现，这是一颗周期为$P = 3.34395390\pm0.00000020$ d的分离双线M型矮双星，具有日全食。我们结合了TRES/FLWO 1.5 m的径向速度（RV）测量，以及HATNet、FLWO 1.2 m、BOS 0.8 m和NASA K2 Campaign 5的时间序列测光，以确定组成恒星$M_{A} = 0.448\pm0.011$ $M_{\odot}$、$M_{B} = 0.2721^{+0.0041}_{-0.0042}$ $M_{\odot}$、$R_{A} = 0.4548^{+0.0035}_{-0.0036}$ $R_{\odot}$和$R_{B} = 0.2913^{+0.0023}_{-0.0024}$ $R_{\odot}$的质量和半径。我们获得了一个火/麦哲伦近红外光谱的主星在一个完整的二次日食，并使用此来获得解开光谱的两个组件。我们确定了主星ST $_{A} = {\rm M}3.71\pm0.69$和主星ST $_{B} = {\rm M}5.01\pm0.73$的光谱类型，以及主星T $_{\rm eff,A} = 3190\pm110$ K和主星T $_{\rm eff,B} = 3100\pm110$ K的有效温度。我们还测量了[Fe/H] $=+0.298\pm0.080$的金属丰度的系统。我们发现，该系统有一个小的，但显着的，非零偏心率的$0.0136\pm0.0026$。K2光变曲线在周期为$3.41315^{+0.00030}_{-0.00032}$ d时表现出相干变化，该周期略长于轨道周期，我们证明它来自主星。我们将其解释为主要的旋转周期。我们进行定量比较达特茅斯恒星演化模型和七个系统，包括HAT-TR-318-007，其中包含M矮星与$0.2 M_{\odot} < M < 0.5 M_{\odot}$，有金属丰度测量，并确定质量和半径优于5%的精度。发现三个系统的预测和观察到的质量和半径之间的差异。

英文摘要：

We report the discovery by the HATNet survey of HAT-TR-318-007, a $P = 3.34395390\pm0.00000020$ d period detached double-lined M-dwarf binary with total secondary eclipses. We combine radial velocity (RV) measurements from TRES/FLWO 1.5 m, and time-series photometry from HATNet, FLWO 1.2 m, BOS 0.8 m and NASA K2 Campaign 5, to determine the masses and radii of the component stars: $M_{A} = 0.448\pm0.011$ $M_{\odot}$, $M_{B} = 0.2721^{+0.0041}_{-0.0042}$ $M_{\odot}$, $R_{A} = 0.4548^{+0.0035}_{-0.0036}$ $R_{\odot}$, and $R_{B} = 0.2913^{+0.0023}_{-0.0024}$ $R_{\odot}$. We obtained a FIRE/Magellan near-infrared spectrum of the primary star during a total secondary eclipse, and use this to obtain disentangled spectra of both components. We determine spectral types of ST$_{A} = {\rm M}3.71\pm0.69$ and ST$_{B} = {\rm M}5.01\pm0.73$, and effective temperatures of T$_{\rm eff,A} = 3190\pm110$ K and T$_{\rm eff,B} = 3100\pm110$ K, for the primary and secondary star, respectively. We also measure a metallicity of [Fe/H]$=+0.298\pm0.080$ for the system. We find that the system has a small, but significant, non-zero eccentricity of $0.0136\pm0.0026$. The K2 light curve shows a coherent variation at a period of $3.41315^{+0.00030}_{-0.00032}$ d, which is slightly longer than the orbital period, and which we demonstrate comes from the primary star. We interpret this as the rotation period of the primary. We perform a quantitative comparison between the Dartmouth stellar evolution models and the seven systems, including HAT-TR-318-007, that contain M dwarfs with $0.2 M_{\odot} < M < 0.5 M_{\odot}$, have metallicity measurements, and have masses and radii determined to better than 5% precision. Discrepancies between the predicted and observed masses and radii are found for three of the systems.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑