Spectral Line Variability in Be and Bn Stars

高温快速旋转“B”型的光谱吸收线 星星显示出旅行的“颠簸”， 时间 虽然这些突起最初被认为是周期性移动的 以一种可预测的方式，导致一种解释， 新的数据表明， 这些突起经常消失。 为了判断这是否 明显的不可预测性是由不同的“跳动”造成的。 脉动模式或由非周期性现象，长串的 需要光谱数据。 在过去，长期的“运动” 由于实际的时间安排， 国家设施的分配问题。 1992年初，格鲁吉亚 国家将投入运行其新的光谱“多- 望远镜望远镜。该设施将有一个大的有效 聚光电源和电荷耦合器件检测器， 将允许PI获得大量数据进行检查 快速旋转中“轮廓凸点”现象的出现频率 B星，并确定其周期性质。 PI还认为， 这个庞大的数据库将使他能够确定 非径向脉动是否是造成偶发性质量损失的原因 在神秘的快速旋转的Be星群中

The spectral absorption lines of hot, rapidly rotating "B" type stars show traveling "bumps" which travel across the lines with time. Although these bumps were first thought to move periodically in a predictable way, leading to an interpretation that traveling waves (nonradial pulsations) were responsible, new data indicate that the bumps are often missing. In order to judge whether this apparent unpredictability is caused by the "beating" of different pulsation modes or by an aperiodic phenomenon, long strings of spectroscopic data are needed. In the past long "campaigns" have been difficult to undertake because of practical scheduling and allocation problems at national facilities. In early 1992 Georgia State will put into operation its new spectroscopic "Multi- Telescope Telescope. This facility will have a large effective light gathering power and a Charged-Couple Device detector and will permit the PI to obtain large amounts of data to examine the frequency of the "profile bump" phenomenon in rapidly rotating B stars and to ascertain its periodic nature. The PI also believes that the large database assembled will enable him to determine whether nonradial pulsations are responsible for episodic mass loss in the enigmatic group of rapidly rotating "Be" stars.