重力模式作为区分氢燃烧与氦燃烧红巨星的方法
太阳与恒星天体物理
2015-05-27 v1
摘要
红巨星是演化星，其核心的氢已经耗尽，转而在周围的壳层中燃烧氢。一旦红巨星演化到足够程度，核心的氦也会发生聚变。我们在理解红巨星时面临的突出问题包括：对氦点火前表面质量损失量的不确定，以及由旋转和其他过程引起的内部混合量的不确定。由于我们无法区分核心燃烧氦的红巨星和仍然仅在壳层中燃烧氢的红巨星，阻碍了研究的进展。星震学提供了一条前进的道路，它是一种利用恒星自然振荡频率探测其内部结构的强大工具。在此，我们报告了在红巨星中观测到的重力模式周期间距，这使得区分演化阶段成为可能。我们使用Kepler太空望远镜在一年多时间里获得的高精度测光数据，测量了数百颗红巨星的振荡。我们发现许多恒星的偶极模式显示出具有近似规则周期间距的序列。这些恒星分为两个明显的群组，使我们能够明确区分氢壳层燃烧星（周期间距主要约为50秒）和那些同时燃烧氦的星（周期间距约为100至300秒）。
引用
@article{arxiv.1103.5805,
title = {Gravity modes as a way to distinguish between hydrogen- and helium-burning red giant stars},
author = {Timothy R. Bedding and Benoit Mosser and Daniel Huber and Josefina Montalban and Paul Beck and Joergen Christensen-Dalsgaard and Yvonne P. Elsworth and Rafael A. Garcia and Andrea Miglio and Dennis Stello and Timothy R. White and Joris De Ridder and Saskia Hekker and Conny Aerts and Caroline Barban and Kevin Belkacem and Anne-Marie Broomhall and Timothy M. Brown and Derek L. Buzasi and Fabien Carrier and William J. Chaplin and Maria Pia Di Mauro and Marc-Antoine Dupret and Soeren Frandsen and Ronald L. Gilliland and Marie-Jo Goupil and Jon M. Jenkins and Thomas Kallinger and Steven Kawaler and Hans Kjeldsen and Savita Mathur and Arlette Noels and Victor Silva Aguirre and Paolo Ventura},
journal= {arXiv preprint arXiv:1103.5805},
year = {2015}
}
备注
to appear as a Letter to Nature