Mass Loss in Evolved Stars
Mass Loss in Evolved Stars
复制标题
DOI：
10.1017/s1743921323002788
复制
发表时间：
2022-12
期刊：
影响因子：
--
通讯作者：
L. Matthews
中科院分区：
文献类型：
--
作者：
L. Matthews
摘要在渐近巨星分支（AGB）演化阶段，低速冷风引起的剧烈质量损失是中低质量恒星的一个显著特征。这样的风会将初始恒星质量的80%返回到星际介质中，并在使其富含尘埃和重元素方面发挥重要作用。理解AGB质量损失背后的物理学的一个挑战是它依赖于复杂和高度动态过程之间的相互作用，包括脉动，对流，冲击，磁场和尘埃和分子形成引起的不透明度变化。我强调了我们对后期恒星质量损失的理解的最新进展的一些例子，这些进展来自无线电和（亚）毫米观测，特别关注那些在空间，时间和频率上解决演化恒星的表面和扩展大气的进展。
Abstract Intense mass loss through cool, low-velocity winds is a defining characteristic of low-to-intermediate mass stars during the asymptotic giant branch (AGB) evolutionary stage. Such winds return up ∼80% of the initial stellar mass to the interstellar medium and play a major role in enriching it with dust and heavy elements. A challenge to understanding the physics underlying AGB mass loss is its dependence on an interplay between complex and highly dynamic processes, including pulsations, convective flows, shocks, magnetic fields, and opacity changes resulting from dust and molecule formation. I highlight some examples of recent advances in our understanding of late-stage stellar mass loss that are emerging from radio and (sub)millimeter observations, with a particular focus on those that resolve the surfaces and extended atmospheres of evolved stars in space, time, and frequency.