This program was begun under Prof. Charles Schweighauser to simultaneously monitor the photometric and spectroscopic fluctuations of bright Be Stars. A Be star is a star that is much hotter and more massive than our Sun which has emission lines in it spectrum due to a disk of material accumulated from its stellar wind. Our current program is focused on the long-term monitoring of Psi Persei, 59 Cyg, Kappa Draconis, and 66 Oph. We are looking for patterns of behavior in these stars that will help to explain the mechanism that produces the strong emission lines in their spectra.
The following are a list of Be Stars that are or have been active targets in our observing program since 2006.
Last Updated 2024 June 4