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K.S. Bjorkman, A.S. Miroshnichenko (U. Toledo)
The bright (V=2.3) B0.3IV star \delta~Sco (HD~143275; HR~5953) was proposed as a Be star by Coté & van Kerkwijk (1990) on the basis of mild emission wings flanking an H\alpha absorption core. Previously published spectra of the star showed no evidence of emission. During the summer of 2000, \delta~Sco entered a true H\alpha emission phase (Fabregat, IAUC 7461). Using the Ritter Observatory 1-m telescope and échelle spectrograph, we monitored the spectroscopic development of the Be outburst from early August through early October 2000, when the star became too low in the sky for observations from Toledo. A total of 19 observations were obtained over the span of 55 days. We present preliminary results from our spectroscopy, and discuss possible implications for the suspected binary system.
Partial support for this research has been provided under NASA grant NAG5-8054. KSB is a Cottrell Scholar of the Research Corporation, and gratefully acknowledges their support.
The author(s) of this abstract have provided an email address for comments about the abstract: karen@astro.utoledo.edu