利用陀螺年代学研究说明性场星的年龄：可行性、局限性和误差
Ages for illustrative field stars using gyrochronology: viability, limitations and errors
摘要：
我们在这里开发了一种改进的方法，使用旋转的恒星作为时钟，使用太阳设置它，并证明它能很好地保持时间。这种称为陀螺年代学的技术，允许仅使用自转周期和颜色来推导太阳型和晚型主序星的年龄。该技术在这里澄清和发展，并用于推导年龄说明组附近，晚型场星测量旋转周期。我们首先证明了现实的接口序列，使技术成为可能的集群和场星的旋转观测的统一功能，并将其扩展到Skumanich的建议之外，指定这些恒星的旋转质量依赖性。我们先确定哪些恒星目前还不能使用，然后用太阳来校准年龄依赖性。传播误差以了解它们对颜色和周期的依赖性。与该技术相关的代表性年龄误差估计为~15%（加上可能的系统误差）晚F，G，K和早M星。通过Gyrochronology获得的Mt.威尔逊星被证明是在很好的协议与色球年龄的所有，但最蓝的恒星，并可能优于。陀螺仪年龄，然后计算每一个活跃的主序星领域的研究斯特拉斯迈尔和合作者在其他年龄是不可用的。这些被证明是大多数小于1Gyr，与平均年龄为3.65亿年。Pizzolato及其合作者收集的单个晚型主序星的样本进行了评估，并显示其陀螺年龄范围从1亿年到几个Gyr，中位年龄为1.2 Gyr。最后，我们证明了三个宽双星XiBooAB，61 CygAB，和AlphaCenAB的各个组成部分产生基本相同的陀螺仪年龄。
英文摘要：
We here develop an improved way of using a rotating star as a clock, set it using the Sun, and demonstrate that it keeps time well. This technique, called gyrochronology, permits the derivation of ages for solar- and late-type main sequence stars using only their rotation periods and colors. The technique is clarified and developed here, and used to derive ages for illustrative groups of nearby, late-type field stars with measured rotation periods. We first demonstrate the reality of the interface sequence, the unifying feature of the rotational observations of cluster and field stars that makes the technique possible, and extends it beyond the proposal of Skumanich by specifying the mass dependence of rotation for these stars. We delineate which stars it cannot currently be used on. We then calibrate the age dependence using the Sun. The errors are propagated to understand their dependence on color and period. Representative age errors associated with the technique are estimated at ~15% (plus possible systematic errors) for late-F, G, K, & early-M stars. Ages derived via gyrochronology for the Mt. Wilson stars are shown to be in good agreement with chromospheric ages for all but the bluest stars, and probably superior. Gyro ages are then calculated for each of the active main sequence field stars studied by Strassmeier and collaborators where other ages are not available. These are shown to be mostly younger than 1Gyr, with a median age of 365Myr. The sample of single, late-type main sequence field stars assembled by Pizzolato and collaborators is then assessed, and shown to have gyro ages ranging from under 100Myr to several Gyr, and a median age of 1.2Gyr. Finally, we demonstrate that the individual components of the three wide binaries XiBooAB, 61CygAB, & AlphaCenAB yield substantially the same gyro ages.
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