恒星自转：从ONC到太阳
Stellar spindown: From the ONC to the Sun
摘要：
自转是恒星演化的一个关键参数。从100万年（ONC的年龄）到4.5 Gyr（太阳的年龄），类太阳恒星会失去大约1-2个数量级的特定角动量。这种旋转制动的主要因素被认为是恒星与磁盘的相互作用和磁力驱动的恒星风。在过去的十年里，探测恒星自旋下降的观测基础已经有了很大的改善。在探索旋转制动的潜在物理原因方面取得了重大进展。参数化模型结合的影响，星盘相互作用，风，和前主序星收缩能够再现的主要特征的旋转数据的恒星跨越3个数量级以上的年龄。这使我们能够根据自转速率来限制恒星的年龄（“陀螺年代学”）。未来工作的一个主要挑战是将这种类型的分析扩展到亚恒星质量范围，其中旋转数据库仍然稀疏。需要更多的理论和观测工作来探索制动过程的物理学，旨在从第一原理解释旋转演化。在这篇关于Cool Stars 15的评论中，我将总结该领域的现状和最近的发展。
英文摘要：
Rotation is a key parameter in the evolution of stars. From 1 Myr (the age of the ONC) to 4.5 Gyr (the age of the Sun), solar-like stars lose about 1-2 orders of specific angular momentum. The main agents for this rotational braking are believed to be star-disk interaction and magnetically powered stellar winds. Over the last decade, the observational fundament to probe the stellar spindown has dramatically improved. Significant progress has been made in exploring the underlying physical causes of the rotational braking. Parameterized models combining the effects of star-disk interaction, winds, and pre-main sequence contraction are able to reproduce the main features of the rotational data for stars spanning more than 3 orders of magnitude in age. This has allowed us to constrain stellar ages based on the rotation rates ('gyrochronology'). One main challenge for future work is to extend this type of analysis to the substellar mass range, where the rotational database is still sparse. More theoretical and observational work is required to explore the physics of the braking processes, aiming to explain rotational evolution from first principles. In this review for Cool Stars 15, I will summarize the status quo and the recent developments in the field.
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