OBSERVATIONAL SIGNATURES OF CONVECTIVELY DRIVEN WAVES IN MASSIVE STARS
OBSERVATIONAL SIGNATURES OF CONVECTIVELY DRIVEN WAVES IN MASSIVE STARS
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DOI：
10.1088/2041-8205/806/2/l33
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发表时间：
2015-06-20
影响因子：
7.9
通讯作者：
Rogers, T. M.
中科院分区：
文献类型：
--
作者：
Aerts, C.;Rogers, T. M.
我们证明了用高精度CoRoT空间光度计观测到的年轻大质量O型恒星中存在对流驱动内重力波(IGW)的观测证据。这一证据来自于基于差动旋转大质量恒星中IGW的二维流体动力学模拟的速度谱与观测光谱的比较。我们还表明，IGW引起的速度谱可能导致可检测到的线型变率，并解释了OB星观测线型中出现宏观湍流的原因。我们的发现提供了预测，通过将明亮、缓慢和快速旋转的OB型恒星样本纳入K2任务的科学计划，并伴随着高精度光谱，以及它们与不同质量和年龄的IGW的多维流体动力学模拟的对抗，可以很容易地验证这些预测。
We demonstrate observational evidence for the occurrence of convectively driven internal gravity waves (IGWs) in young massive O-type stars observed with high-precision CoRoT space photometry. This evidence results from a comparison between velocity spectra based on two-dimensional hydrodynamical simulations of IGWs in a differentially rotating massive star and the observed spectra. We also show that the velocity spectra caused by IGWs may lead to detectable line-profile variability and explain the occurrence of macroturbulence in the observed line profiles of OB stars. Our findings provide predictions that can readily be tested by including a sample of bright, slowly and rapidly rotating OB-type stars in the scientific program of the K2 mission accompanied by high-precision spectroscopy and their confrontation with multi-dimensional hydrodynamic simulations of IGWs for various masses and ages.