利用高角分辨率成像定量恒星质量损失
Quantifying Stellar Mass Loss with High Angular Resolution Imaging
摘要：
物质在宇宙中不断循环。最强大的回收途径之一是通过恒星质量损失。所有的恒星都表现出质量损失的速率在~10（-14）到10（-4）M（太阳）yr-1之间，取决于光谱类型、光度等级、自转速率、伴星接近度和演化阶段。第一代恒星主要由氢和氦组成。这些物质通过大质量的风、行星状星云和超新星爆炸，在星际介质中播撒了更重的元素。随后的几代恒星吸收了这种物质，改变了恒星的燃烧方式，并为行星形成提供了物质。了解质量损失对于建模单个恒星以及回答更大的天体物理问题至关重要。了解质量损失对于跟踪单星、双星、星团和星系的演化至关重要。质量损失是我们在模拟基本恒星过程中最薄弱的领域之一。这在很大程度上是由于缺乏对恒星光球和质量损失过程的详细观测。望远镜阵列的高分辨率光学成像开始提供这些数据，并与光谱学和宽红外和亚毫米覆盖相结合，支持更复杂的模型在快速计算机上，并有望在质量损失研究的新时代。
英文摘要：
Mass is constantly being recycled in the universe. One of the most powerful recycling paths is via stellar mass-loss. All stars exhibit mass loss with rates ranging from ~10(-14) to 10(-4) M(sun) yr-1, depending on spectral type, luminosity class, rotation rate, companion proximity, and evolutionary stage. The first generation of stars consisted mostly of hydrogen and helium. These shed material - via massive winds, planetary nebulae and supernova explosions - seeding the interstellar medium with heavier elements. Subsequent generations of stars incorporated this material, changing how stars burn and providing material for planet formation. An understanding of mass loss is critical for modeling individual stars as well as answering larger astrophysical questions. Understanding mass loss is essential for following the evolution of single stars, binaries, star clusters, and galaxies. Mass loss is one of our weakest areas in the modeling of fundamental stellar processes. In large part this is owing to lack of confrontation with detailed observations of stellar photospheres and the mass-loss process. High resolution optical imagery with telescope arrays is beginning to provide these data and, combined with spectroscopy and broad infrared and sub-mm coverage, supporting more sophisticated models on fast computers and promising a new era in mass-loss studies.
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