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Low frequency ($\nu\lesssim 150\,$MHz) stellar radio emission is expected tooriginate in the outer corona at heights comparable to and larger than thestellar radius. Such emission from the Sun has been used to study coronalstructure, mass ejections, space-weather conditions around the planets (Schwenn2006). Searches for low-frequency emission from other stars have only detecteda single active flare-star (Lynch et al. 2017) that is not representative ofthe wider stellar population. Here we report the detection of low-frequencyradio emission from a quiescent star, GJ 1151--- a member of the most commonstellar type (red dwarf or spectral class M) in the Galaxy. The characteristicsof the emission are similar to those of planetary auroral emissions (Zarka1998) (e.g. Jupiter's decametric emission), suggesting a coronal structuredominated by a global magnetosphere with low plasma density. Our results showthat large-scale currents that power radio aurorae operate over a vast range ofmass and atmospheric composition, ranging from terrestrial planets tomain-sequence stars. The Poynting flux required to produce the observed radioemission cannot be generated by GJ 1151's slow rotation, but can originate in asub-Alfv\'{e}nic interaction of its magnetospheric plasma with a short-periodexoplanet. The emission properties are consistent with theoretical expectations(Zarka 2007; Lanza 2009; Saur et al. 2013; Turnpenney et al. 2018) forinteraction with an Earth-size planet in a $\sim 1-5$ day-long orbit.

Coherent radio emission from a quiescent red dwarf indicative of star-planet interaction