Spectral Line Variability in Be and Bn Stars

Be 和 Bn 星的谱线变化

• 批准号: 9115121
• 负责人: Douglas Gies
• 金额: $ 9万
• 依托单位: Georgia State University
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1992
• 资助国家: 美国
• 起止时间: 1992-03-01 至 1995-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9115121&HistoricalAwards=false
• 关键词: Spectral; Line; Variability; Bn; Stars

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.

热旋转的“ B”型恒星的光谱吸收线显示行进的“颠簸”，这些恒星随着时间的流逝而跨线传播。 尽管首先认为这些颠簸会以可预测的方式定期移动，但导致一种解释，即行进波（非自由搏动）是负责的，但新数据表明颠簸经常缺失。 为了判断这种明显的不可预测性是由不同的脉动模式的“殴打”引起的，还是由于需要长的光谱数据而引起的。 在过去的长期以来，由于在国家设施的实际日程安排和分配问题，很难进行“运动”。 在1992年初，佐治亚州将在其新的光谱型“多望远镜望远镜”中运作。该设施将具有很大的有效的轻聚集能力和带电的套管设备探测器，并将PI允许大量数据获得迅速旋转的bump and Obles the Onder the Ordister persubl of the Piciby piciby piciby pi seception pi seceptable serge的频率，以构成pi的频率。确定在迅速旋转的“ BE”恒星的神秘群体中，非自由搏动是否负责发作的质量损失。