Low frequency ( \nu \lesssim 150 MHz ) stellar radio emission is expected to originate in the outer corona at heights comparable to and larger than the stellar radius .
Such emission from the Sun has been used to study coronal structure , mass ejections , space-weather conditions around the planets \citep schwenn-2006 .
Searches for low-frequency emission from other stars have only detected a single active flare-star \citep lynch-2017 that is not representative of the wider stellar population .
Here we report the detection of low-frequency radio emission from a quiescent star , GJ 1151— a member of the most common stellar type ( red dwarf or spectral class M ) in the Galaxy .
The characteristics of the emission are similar to those of planetary auroral emissions \citep zarka-1998 ( e.g .
Jupiter ’ s decametric emission ) , suggesting a coronal structure dominated by a global magnetosphere with low plasma density .
Our results show that large-scale currents that power radio aurorae operate over a vast range of mass and atmospheric composition , ranging from terrestrial planets to main-sequence stars .
The Poynting flux required to produce the observed radio emission can not be generated by GJ 1151 ’ s slow rotation , but can originate in a sub-Alfvénic interaction of its magnetospheric plasma with a short-period exoplanet .
The emission properties are consistent with theoretical expectations \citep zarka-2007 , lanza-2009 , saur-2013 , turnpenney-2018 for interaction with an Earth-size planet in a \sim 1 - 5 day-long orbit .