AI 中文总结
本研究通过高分辨率光谱观测，在RS CVn型恒星白羊座UX的长寿命光学耀斑中检测到可能的恒星CME，其速度、质量等参数支持该CME的存在，为恒星CME的观测提供了新证据。
AI 中文摘要
日冕物质抛射（CME）是恒星日冕中磁化等离子体的大规模爆发，且总是伴随耀斑出现。本研究呈现了对RS CVn型恒星白羊座UX（UX Ari）上长寿命光学耀斑的高分辨率光谱观测。在耀斑峰值附近，研究人员在Hα线轮廓中检测到远蓝移发射成分——这是爆发日珥的特征，表明存在可能的恒星CME。校正投影效应后，若假设为径向传播，爆发速度达约-432 km s⁻¹，显著超过主成分的逃逸速度（约304 km s⁻¹），这有力支持了恒星CME的检测。该CME的质量至少为2.7×10²⁰ g，动能为2.5×10³⁵ erg；质量值与太阳耀斑-CME标度关系一致，动能低于太阳趋势。耀斑本身在Hα中释放的能量为4.2×10³⁶ erg，对应白光热辐射能量约为2.8×10³⁸ erg。在整个耀斑事件中，Hα轮廓的演化不对称性揭示了复杂的等离子体动力学。
英文摘要
Coronal mass ejections (CMEs) are large-scale eruptions of magnetized plasma from stellar coronae, and they are always accompanied by flares. In this study, we present high-resolution spectroscopic observations of a long-duration optical flare on the RS CVn-type star UX Arietis (UX Ari). Around the flare peak, we have detected a far-blueshifted emission component in the H$α$ line profile---a signature of an erupting prominence---indicating a possible stellar CME. After correcting for projection effects, the eruption velocity reaches $\sim -432$ km s$^{-1}$ when assuming radial propagation, significantly exceeding the escape velocity of the primary component ($\approx 304$ km s$^{-1}$). This strongly supports the detection of a stellar CME. The mass of this CME is at least $2.7 \times 10^{20}$ g, and its kinetic energy is $2.5 \times 10^{35}$ erg. The mass value is consistent with the solar flare--CME scaling relation, while its kinetic energy lies below the solar trend. The flare itself released an energy of $4.2 \times 10^{36}$ erg in the H$α$, corresponding to a white-light bolometric energy of roughly $2.8 \times 10^{38}$ erg. Throughout the flaring event, evolving asymmetries in the H$α$ profile reveal complex plasma dynamics.
Journal ref2026ApJ..1005..187C
