Abstract
A study using archive IUE data of time-varying mass loss has been carried out for a sample of 12 supergiants in the spectral range B5–B9. Additionally dedicated IUE velocity-time observations of ‘discrete absorption components’ (DAC) in the UV resonance lines have been made for one of the stars (βOri), while optical data obtained for this star shows time variability in the Hα profile. Ions in which mass-loss features occur are unambiguously identified by comparing spectra of the stars at different mass loss episodes. Time variability in the mass-loss activity of late B-type supergiants is discussed and the stars are examined for trends with effective temperature. The basis for a theoretical model of the stellar wind in these stars is introduced.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
