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Context: Active M dwarfs frequently exhibit large flares, which can pose anexistential threat to the habitability of any planet in orbit in addition tomaking said planets more difficult to detect. M dwarfs do not lose angularmomentum as easily as earlier-type stars, which maintain the high levels ofstellar activity for far longer. Studying young, fast-rotating M dwarfs is keyto understanding their near stellar environment and the evolution of activityAims: We study stellar activity on the fast-rotating M dwarf GJ 3270. Methods:We analyzed dedicated high cadence, simultaneous, photometric andhigh-resolution spectroscopic observations obtained with CARMENES of GJ 3270over 7.7 h, covering a total of eight flares of which two are strong enough tofacilitate a detailed analysis. We consult the TESS data, obtained in the monthprior to our own observations, to study rotational modulation and to comparethe TESS flares to those observed in our campaign. Results: The TESS dataexhibit rotational modulation with a period of 0.37 d. The strongest flarecovered 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 ofabout 10,000 K. The flare also leaves clear marks in the spectral time series.In particular, we observe an evolving, mainly blue asymmetry in chromosphericlines, which we attribute to a post-flare, corotating feature. To our knowledgethis is the first time such a feature has been seen on a star other than ourSun. Conclusions: Our photometric and spectroscopic time series covers theeruption of a strong flare followed up by a corotating feature analogous to apost-flare arcadal loop on the Sun with a possible failed ejection of material.

Simultaneous photometric and CARMENES spectroscopic monitoring of fast-rotating M dwarf GJ 3270. Discovery of a post-flare corotating feature