Radio Continuum Observations of Active Stars

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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.