标题： 恒星上的磁场 显示英文标题

标题： Magnetic Fields on Cool Stars

摘要： 磁场是冷却星物理的重要组成部分，测量磁场及其几何结构具有重要意义，以理解恒星发电机及其对恒星形成和恒星演化的影响。 在过去的几年中，大量磁场测量数据已经可用。 目前有两种主要方法用于测量冷却星中的塞曼效应; 1) 测量偏振光，例如用于生成磁场图，2) 测量综合塞曼展宽以测量恒星表面的平均磁场强度。 本文简要回顾了这两种方法，并比较了现在大约十几颗M型星的相关结果。 似乎我们在活跃的M型星中看到了各种各样的磁场几何结构和场强，典型的平均场强为几kG。 然而，对几何结构的解释尚未导致对磁场发电机和场配置的清晰图像，需要更多的观测数据，也需要对我们测量的基本理解进行研究。 显示英文摘要

摘要： Magnetic fields are an important ingredient to cool star physics, and there is great interest in measuring fields and their geometry in order to understand stellar dynamos and their influence on star formation and stellar evolution. During the last few years, a large number of magnetic field measurements became available. Two main approaches are being followed to measure the Zeeman effect in cool stars; 1) the measurement of polarized light, for example to produce magnetic maps, and 2) the measurement of integrated Zeeman broadening to measure the average magnetic field strength on the stellar surface. This article briefly reviews the two methods and compares results between them that are now available for about a dozen M-type stars. It seems that we see a great variety of magnetic geometries and field strengths with typical average fields of a few kG in active M-type stars. The interpretation of geometries, however, has not yet led to a clear picture of magnetic dynamos and field configuration, and work is needed on more observational data but also on the fundamental understanding of our measurements.