对快速旋转的M矮星GJ 3270的同时光度和CARMENES光谱监测。耀斑后共转特征的发现
Simultaneous photometric and CARMENES spectroscopic monitoring of fast-rotating M dwarf GJ 3270. Discovery of a post-flare corotating feature
摘要：
内容：活跃的M矮星经常会出现大的耀斑，这可能会对轨道上任何行星的可居住性构成威胁，除了使所述行星更难以探测。M型矮星不像早期类型的恒星那样容易失去角动量，早期类型的恒星保持高水平的恒星活动的时间要长得多。研究年轻、快速旋转的M矮星是了解其近星环境和活动演化的关键。目的：研究快速旋转的M矮星GJ 3270上的恒星活动。研究方法：我们分析了专用的高节奏，同时，光度和高分辨率的光谱观测与CARMENES的GJ 3270超过7.7小时，共涵盖8个耀斑，其中两个是足够强大，以方便详细的分析。我们参考了在我们自己观测之前一个月获得的TESS数据，以研究旋转调制，并将TESS耀斑与我们观测到的耀斑进行比较。结果：TESS数据呈现旋转调制，周期为0.37d。我们的观测活动所覆盖的最强耀斑释放的总能量约为3.6e32尔格，接近超级耀斑状态。这个耀斑在B、V、r、i和z光度带中可见，这使我们能够确定大约10，000 K的峰值温度。耀斑也在光谱时间序列中留下了清晰的痕迹。特别是，我们观察到一个不断发展的，主要是蓝色的不对称色球线，我们归因于耀斑后，共转功能。据我们所知，这是第一次在太阳以外的恒星上看到这样的特征。结论：我们的光度和光谱时间序列涵盖了一个强大的耀斑爆发，随后由一个共转功能类似于一个后耀斑arcadal环太阳上的一个可能失败的喷射材料。
英文摘要：
Context: Active M dwarfs frequently exhibit large flares, which can pose an existential threat to the habitability of any planet in orbit in addition to making said planets more difficult to detect. M dwarfs do not lose angular momentum as easily as earlier-type stars, which maintain the high levels of stellar activity for far longer. Studying young, fast-rotating M dwarfs is key to understanding their near stellar environment and the evolution of activity Aims: We study stellar activity on the fast-rotating M dwarf GJ 3270. Methods: We analyzed dedicated high cadence, simultaneous, photometric and high-resolution spectroscopic observations obtained with CARMENES of GJ 3270 over 7.7 h, covering a total of eight flares of which two are strong enough to facilitate a detailed analysis. We consult the TESS data, obtained in the month prior to our own observations, to study rotational modulation and to compare the TESS flares to those observed in our campaign. Results: The TESS data exhibit rotational modulation with a period of 0.37 d. The strongest flare covered by our observing campaign released a total energy of about 3.6e32 erg, putting it close to the superflare regime. This flare is visible in the B,V, r, i, and z photometric bands, which allows us to determine a peak temperature of about 10,000 K. The flare also leaves clear marks in the spectral time series. In particular, we observe an evolving, mainly blue asymmetry in chromospheric lines, which we attribute to a post-flare, corotating feature. To our knowledge this is the first time such a feature has been seen on a star other than our Sun. Conclusions: Our photometric and spectroscopic time series covers the eruption of a strong flare followed up by a corotating feature analogous to a post-flare arcadal loop on the Sun with a possible failed ejection of material.
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