Stellar multiplicity and stellar rotation: insights from APOGEE
Stellar multiplicity and stellar rotation: insights from APOGEE
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恒星多重性和恒星自转：APOGEE 的见解
DOI：
10.1093/mnras/stac590
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发表时间：
2022
影响因子：
4.8
通讯作者：
Majewski, Steven
中科院分区：
文献类型：
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作者：
Daher, Christine Mazzola;Badenes, Carles;Tayar, Jamie;Pinsonneault, Marc;Koposov, Sergey E.;Kratter, Kaitlin;Moe, Maxwell;Anguiano, Borja;Godoy-Rivera, Diego;Majewski, Steven
我们测量旋转展宽的光谱所采取的阿帕奇点天文台银河演化实验（APOGEE）调查，以表征恒星的多重性和旋转之间的关系。我们创建了一个2786颗巨星和24496颗矮星的样本，这些巨星和矮星具有来自APOGEE管道的恒星参数和多个径向速度，从我们自己的管道中确定的投影旋转速度svsini，以及Sanders & Das测量的距离，质量和年龄。我们使用径向速度最大偏移的统计分布ΔRVmax作为密近双星分数的代表，以探索恒星演化，旋转和多重性之间的相互作用。假设最小轨道周期是Roche瓣溢出和旋转同步的临界周期，计算了期望vsini和Δ RVmax值的理论上限。这些预期与我们样本中观察到的最大Δ RVmax和vsini值之间的正相关性一致，作为log（g）的函数。我们发现，在我们的样本中的快速旋转有很高的发生率短周期[log（P/d）<$4]同伴。我们还发现，老的，快速旋转的主序星有较大的完整性校正密切的二进制分数比年轻的同行。此外，具有大Δ RVmax的快速旋转恒星始终显示预测的陀螺年代学年龄和测量的等时年龄之间存在1-10 Gyr的差异。这些结果指向通过潮汐相互作用的快速旋转和紧密双星之间的联系。我们的结论是，恒星自转是强烈相关的恒星多重性的领域，并应谨慎的应用程序中的gyrochronology关系到冷星。
We measure rotational broadening in spectra taken by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey to characterize the relationship between stellar multiplicity and rotation. We create a sample of 2786 giants and 24 496 dwarfs with stellar parameters and multiple radial velocities from the APOGEE pipeline, projected rotation speedsvsinidetermined from our own pipeline, and distances, masses, and ages measured by Sanders & Das. We use the statistical distribution of the maximum shift in the radial velocities, ΔRVmax, as a proxy for the close binary fraction to explore the interplay between stellar evolution, rotation, and multiplicity. Assuming that the minimum orbital period allowed is the critical period for Roche Lobe overflow and rotational synchronization, we calculate theoretical upper limits on expectedvsiniand ΔRVmaxvalues. These expectations agree with the positive correlation between the maximum ΔRVmaxandvsinivalues observed in our sample as a function of log(g). We find that the fast rotators in our sample have a high occurrence of short-period [log(P/d) ≲ 4] companions. We also find that old, rapidly rotating main-sequence stars have larger completeness-corrected close binary fractions than their younger peers. Furthermore, rapidly rotating stars with large ΔRVmaxconsistently show differences of 1–10 Gyr between the predicted gyrochronological and measured isochronal ages. These results point towards a link between rapid rotation and close binarity through tidal interactions. We conclude that stellar rotation is strongly correlated with stellar multiplicity in the field, and caution should be taken in the application of gyrochronology relations to cool stars.