Active late-type stars and the applicability of coronal loop models

摘要

Far ultraviolet IUE observations of a sample of solar type stars were combined with existing soft X-ray measurements obtained by HEAO B. The resulting data set was utilized and a new coronal loop model numerical code was developed to perform a preliminary investigation of the applicability of coronal loop models to solar-type stars. Reasonable agreement was found to exist between the predictions of single-component coronal loop model atmospheres. It was demonstrated that semi-empirical, coronal loop models can be applied to account for observed stellar transition region and coronal emission. This result is corroborative evidence for the presence of magnetic field structures analogous to solar coronal loops on the surfaces of solar-type stars. It is suggested that stellar transition region emission arises predominantly from the base of quiescent coronal loop configurations.