论文标题
$α$ persei综合体的恒星旋转和结构：旋律年代学何时开始工作？
Stellar Rotation and Structure of the $α$ Persei Complex: When Does Gyrochronology Start to Work?
论文作者
论文摘要
在预先序列上，太阳状恒星的旋转速率取决于原始磁盘与恒星收缩之间的相互作用。在超过1亿年的年龄（MYR）时，磁性旋转擦除了初始恒星旋转率，并实现了基于旋转的年龄约会（Gyrochonology）。这两个制度之间的过渡之间的确切时间取决于恒星质量，并且由于缺乏可行的校准簇而在经验上挑战。 $α$ Persei Open集群（$ t \ of Yout80 $ Myr，$ d \ of170 $ PC）可能会提供所需的校准器，但是最近对Gaia数据的分析提供了对其年龄和空间范围的观点差异很大。因此，我们分析了Tess，Gaia和Lamost数据的组合，以校准每年$α$的年代，并发现集群的真实形态。通过组装每个成员旋转确认的$α$的列表，我们提供了有力的证据，表明$α$是较大的类似恒星的一部分。通过运动学的背面整合，我们表明，最多的$α$的分散成分五倍近50 Myr。最后，我们利用恒星轮换期来获得相对的陀螺仪年龄，即$α$ 67 $ \ pm的$ \ pm $ 12％，$ 12％的pleiades年龄，鉴于当前的知识，该年龄产生了86美元$ \ pm $ 16。我们表明，到这个年龄段，恒星比$ \ $ \ $ \ $ 0.8 m $ _ {\ odot} $融合以形成一个定义明确的慢序。
On the pre-main-sequence, the rotation rates of Sun-like stars are dictated by the interplay between the protostellar disk and the star's contraction. At ages exceeding 100 million years (Myr), magnetic spin-down erases the initial stellar spin rate and enables rotation-based age dating (gyrochronology). The exact time at which the transition between these two regimes occurs depends on stellar mass, and has been challenging to empirically resolve due to a lack of viable calibration clusters. The $α$ Persei open cluster ($t\approx80$ Myr, $d\approx170$ pc) may provide the needed calibrator, but recent analyses of the Gaia data have provided wildly varying views of its age and spatial extent. As such, we analyze a combination of TESS, Gaia, and LAMOST data to calibrate gyrochronology at the age of $α$ Per and to uncover the cluster's true morphology. By assembling a list of rotationally-confirmed $α$ Per members, we provide strong evidence that $α$ Per is part of a larger complex of similarly-aged stars. Through kinematic back-integration, we show that the most diffuse components of $α$ Per were five times closer together 50 Myr ago. Finally, we use our stellar rotation periods to derive a relative gyrochronology age for $α$ Per of 67 $\pm$ 12% the age of the Pleiades, which yields 86 $\pm$ 16 Myr given current knowledge. We show that by this age, stars more massive than $\approx$0.8 M$_{\odot}$ have converged to form a well-defined slow sequence.
