Angular Momentum Transport in Stellar Interiors
Angular Momentum Transport in Stellar Interiors
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DOI：
10.1146/annurev-astro-091918-104359
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发表时间：
2018-09
影响因子：
33.3
通讯作者：
C. Aerts;S. Mathis;T. Rogers
中科院分区：
文献类型：
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作者：
C. Aerts;S. Mathis;T. Rogers
恒星在出生和死亡之间会失去大量的角动量，这意味着将其从核心转移到表面的有效过程是活跃的。空间星震学提供了一千多颗低质量和中等质量恒星的内部自转速率，揭示了以下事实：在核心氢和核心氦燃烧阶段，单个恒星的自转几乎是均匀的。在红巨星阶段，恒星核心的旋转速度比外壳快10倍。恒星燃烧氦的核心的角动量与白色矮星的角动量一致。观测显示，当恒星有对流核心时，核心角动量会大幅减少。目前的角动量输运理论无法解释这一点。我们建议改进的理论与数据驱动的方法，从而角动量处方来自多维（磁）流体动力学模拟和理论考虑不断测试对现代观测。TESS和PLATO空间任务有可能获得大样本恒星的内部旋转，包括双星和星团中的大质量和贫金属恒星。这将为改进理论和模拟提供强大的观测约束。
Stars lose a significant amount of angular momentum between birth and death, implying that efficient processes transporting it from the core to the surface are active. Space asteroseismology delivered the interior rotation rates of more than a thousand low- and intermediate-mass stars, revealing the following: ▪ Single stars rotate nearly uniformly during the core-hydrogen and core-helium burning phases. ▪ Stellar cores spin up to a factor of 10 faster than the envelope during the red giant phase. ▪ The angular momentum of the helium-burning core of stars is in agreement with the angular momentum of white dwarfs. Observations reveal a strong decrease of core angular momentum when stars have a convective core. Current theory of angular momentum transport fails to explain this. We propose improving the theory with a data-driven approach, whereby angular momentum prescriptions derived frommultidimensional (magneto)hydrodynamical simulations and theoretical considerations are continuously tested against modern observations. The TESS and PLATO space missions have the potential to derive the interior rotation of large samples of stars, including high-mass and metal-poor stars in binaries and clusters. This will provide the powerful observational constraints needed to improve theory and simulations.