Observational characterization of intermediate mass stars

中等质量恒星的观测特征

• 批准号: 8292-2008
• 负责人: Turner, David
• 金额: $ 1.29万
• 依托单位: Saint Mary's University
• 依托单位国家: 加拿大
• 项目类别: Discovery Grants Program - Individual
• 财政年份: 2009
• 资助国家: 加拿大
• 起止时间: 2009-01-01 至 2010-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=420590
• 关键词: Observational; characterization; intermediate; mass; stars

Rich ensembles of stars known as open clusters are beautiful sights in our Galaxy, and the common age, distance, and original chemical composition of their member stars make them ideal calibrators of intrinsic properties (luminosity, temperature, and evolutionary status) for associated objects. Especially important are Cepheid variables, pulsating supergiant stars used as distance indicators to nearby galaxies because the duration of their characteristic brightness cycles relates directly to intrinsic brightness. An additional characteristic described by rate of period change and pulsation amplitude correlates more precisely with their evolutionary status, and may resolve questions about pulsation mode as well. Another common constituent of young clusters are pulsating M supergiants, standard candles in their own right much like Cepheids, but also the last stage of evolution for stars 20-25 times more massive than the Sun prior to their explosion as Type II supernovae. Like Cepheids, the common thread linking such objects is that they represent advanced stages of stellar evolution, where existing observational data can be used to test predictions from increasingly-sophisticated stellar evolutionary models with reality. In the case of M supergiants, it may be possible to detect an observational signature that provides advanced warning of their forthcoming demise.

被称为疏散星团的丰富恒星群是我们银河系中美丽的景象，其成员恒星的共同年龄、距离和原始化学成分使它们成为相关天体内在属性（光度、温度和演化状态）的理想校准器。尤其重要的是造父变星，脉动超巨星用作附近星系的距离指示器，因为它们特征亮度周期的持续时间与内在亮度直接相关。由周期变化率和脉动幅度描述的附加特征与其进化状态更精确地相关，并且也可以解决有关脉动模式的问题。年轻星团的另一个常见组成部分是脉动 M 超巨星，它们本身就是标准烛光，很像造父变星，但也是质量比太阳大 20-25 倍的恒星在爆炸为 II 型超新星之前演化的最后阶段。与造父变星一样，连接这些天体的共同点是它们代表了恒星演化的高级阶段，现有的观测数据可用于测试日益复杂的恒星演化模型的预测与现实。就 M 超巨星而言，有可能检测到观测特征，从而对其即将消亡提供预先警告。