Martínez González, María JesúsAsensio Ramos, AndrésGonzález Fernández, CarlosPino Alemán, Tanausú delMontes Gutiérrez, DavidLuna, ManuelFelipe, TobíasEsteban Pozuelo, SaraLeitzinger, Martin2023-06-222023-06-222022-10-070035-871110.1093/mnras/stac2612https://hdl.handle.net/20.500.14352/72730© 2015 The Authors. This research has been supported by the project PGC-2018-102108- B-100 of the Spanish Ministry of Science and Innovation and by the financial support of MJMG through the Ramón y Cajal fellowship. We also acknowledge the funding received from the European Research Council (ERC) under the European UnionâĂŹs Horizon 2020 research and innovation program (ERC Advanced Grant agreement No. 742265). ML acknowledges the support from Ministerio de Economia, Industria y Competitividad for the Ramón y Cajal fellowship RYC2018-026129-I. TF acknowledges the financial support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant with reference PGC2018-097611-A-I00. M.L. acknowledges the Austrian Science Fund (FWF): P30949-N36.We study the magnetic activity in the ultra fast rotator dMe HK Aqr using tomography techniques with high resolution spectroscopy. We aim to characterise how this magnetic activity appears in a regime of very fast rotation without external forces, given that HK Aqr is, very likely, a single star. We find dark spots located at low latitudes. We also detect prominences below the co-rotation radius and at low latitudes, coinciding with the spot latitudes. This apparent low-latitude activity contrasts with what is typically observed in fast rotators, which tend to form large polar spots. Moreover, we detect a stellar flare which produces an enhancement of the continuum and additional emission in the core of most photospheric and chromospheric lines. We find evidence that the flare is ignited above an active region, as seen in solar flares. This means that, with high probability, the flare is initiated by magnetic reconnection in complex active regions. We also present evidence of bulk red-shifted velocities of about 15 km s^(−1) during the rise of the flare, and velocities of 5-10 km s^(−1) during the decay phase. An estimation of the heating during the flare results in about 200 kK close to the peak and in 100 kK at the end of the observations.engjournal articlehttp://dx.doi.org/10.1093/mnras/stac2612https://academic.oup.comopen access52StarProminencesCoronaAstrofísica