年轻太阳的日冕物质抛射：通过太阳-恒星联系的观测视角
Coronal Mass Ejections from Young Suns: An Observational View through the Solar-Stellar Connection
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中文总结 AI 辅助
本综述聚焦年轻太阳型恒星的日冕物质抛射（CME），以多普勒位移方法为主要观测手段，总结其与太阳现象的相似性、物理性质及对行星空间天气的影响，并展望未来研究方向。
中文摘要 AI 辅助
Kepler和TESS已揭示，磁活动恒星频繁产生耀斑和超级耀斑，这增加了频繁、快速且大规模的日冕物质抛射（CME）可能影响行星空间天气环境的可能性。然而，对恒星CME的观测约束仍然极为有限。几种诊断方法，包括多普勒位移谱线、日冕暗化和射电暴，主要针对冷矮星进行了探索，而最近的观测已开始将这些搜索扩展到年轻太阳型恒星，这些恒星是太阳-恒星联系的重要基准。本综述的目标是总结关于年轻太阳型恒星CME特征的当前理解和近期观测进展，主要关注多普勒位移方法。它考察了这些特征如何与太阳观测和模型相似，推断出的物理性质能告诉我们关于恒星CME的发生及其对恒星质量损失的贡献，以及多普勒位移特征如何与多波长诊断相关联。与冷矮星和密近双星的CME候选体的比较进一步将这些特征置于不同恒星环境中恒星CME的更广泛背景下。这些结果对年轻行星的空间天气环境具有重要意义，同时也指出了未来观测和建模的关键方向。
英文摘要
Kepler and TESS have revealed that magnetically active stars frequently produce flares and superflares, raising the possibility that frequent, fast, and massive coronal mass ejections (CMEs) may affect planetary space weather environments. However, observational constraints on stellar CMEs remain extremely limited. Several diagnostics, including Doppler-shifted spectral lines, coronal dimming, and radio bursts, have been explored mainly for cool dwarfs, while recent observations have begun to extend these searches to young solar-type stars, which serve as important benchmarks for the solar-stellar connection. The goal of this review is to summarize the current understanding and recent observational progress on CME signatures from young solar-type stars, with a primary focus on Doppler-shift methods. It examines how these signatures resemble solar observations and models, what the inferred physical properties can tell us about the occurrence of stellar CMEs and their contribution to stellar mass loss, and how Doppler-shift signatures can be connected with multi-wavelength diagnostics. Comparisons with CME candidates from cool dwarfs and close binaries further place these signatures in the broader context of stellar CMEs in different stellar environments. These results have important implications for the space weather environments of young planets, while also pointing to key directions for future observations and modeling.
发表机构
- The Hakubi Center for Advanced Research, Kyoto University（京都大学白兔高级研究中心）
- Department of Physics, Kyoto University（京都大学物理系）
- Heliophysics Science Division, NASA Goddard Space Flight Center（NASA戈达德太空飞行中心太阳物理学部）
- Department of Physics, The Catholic University of America（美国天主教大学物理系）
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