Spectrographic Observation of Northern Be Stars
Additional Funding Sources
This research was made possible by support from Joe and Frankee Daglen.
Abstract
A Be star is defined as a non-supergiant B star whose spectrum, either in the past or present, contains Balmer emission lines. While rather vague, this definition does encapsulate one of the unique aspects of Be stars: variability in the circumstellar environment. In an effort to investigate these stars and their environments, we obtained high resolution spectra using a 14-inch SCT located at the College of Idaho observatory in Caldwell, Idaho. The spectra were adjusted for instrument response and sensitivity, and wavelength calibrated using a helium-argon lamp. We observed three distinct categories of spectra: pure emission, double-peaked emission and absorption, and double-peaked emission profiles. These distinct profiles are impacted by pulsation of the circumstellar disk, as well as viewing angle of the star relative to its equatorial axis. Further analysis is required to determine additional system parameters.
Spectrographic Observation of Northern Be Stars
A Be star is defined as a non-supergiant B star whose spectrum, either in the past or present, contains Balmer emission lines. While rather vague, this definition does encapsulate one of the unique aspects of Be stars: variability in the circumstellar environment. In an effort to investigate these stars and their environments, we obtained high resolution spectra using a 14-inch SCT located at the College of Idaho observatory in Caldwell, Idaho. The spectra were adjusted for instrument response and sensitivity, and wavelength calibrated using a helium-argon lamp. We observed three distinct categories of spectra: pure emission, double-peaked emission and absorption, and double-peaked emission profiles. These distinct profiles are impacted by pulsation of the circumstellar disk, as well as viewing angle of the star relative to its equatorial axis. Further analysis is required to determine additional system parameters.
Comments
T91