Radio Continuum Observations of Active Stars

在过去的二十年里，大口径无线电的建设 干涉仪提供了一个重要的工具，在了解 几组“日冕”的物理特征 星 两个这样的群体是磁活性较低的主要 序星（像太阳）和非常年轻的（“赤裸的金牛座T”） 恒星的外层已经蒸发掉， 直接观察。 在这项提案中，一位前NSF 总统青年调查员计划进行为期一年的观察 这两组恒星的日冕辐射的调查。 这些无线电数据将与x射线和紫外线数据相结合 以提供对等离子体的物理理解， 在这些恒星的日冕中的耀斑活动。 这个项目 将有助于使秩序，以目前混乱的图片 放射性活跃的恒星，并最终帮助提供 一个广泛的背景下，其中理解的差异和 导致无线电发射的物理过程的相似性 包括太阳在内的几个恒星群

In the last twenty years the construction of large aperture radio interferometers has provided an essential tool in understanding the physical characteristics of the "coronas" of several groups of stars. Two such groups are the magnetically active lower main sequence stars (like the Sun) and very young ("naked T Tauri") stars whose outer envelopes have evaporated away enough to permit their direct observation. In this proposal a former NSF Presidential Young Investigator plans a one year observational survey of emissions from the coronas of these two groups of stars. These radio data will be combined with x-ray and ultraviolet data to provide a physical understanding of the plasma responsible for flaring activity that in the coronas of these stars. This project will help bring order to a currently confused picture of the emission of radio- active stars and should ultimately help provide a broad context within which to understand the differences and similarities of physical processes leading to the radio emissions in several groups of stars, including the Sun.