Almost two decades ago, strong non-thermal variable radio-emission had been detected from θ¹ Orionis A, the third most luminous OB star in the Orion Trapezium Cluster. The source of the emission, has been a puzzling issue since then. Now, it is established that θ¹ Orionis A is a close triple stellar system and that the radio emission originates from the visual companion θ¹ Orionis A2. In this contribution we re-analyse available radio data combined with near-infrared observations in order to constrain the nature of θ¹ Orionis A2. Stringent constraints on the size of the non-thermal radio emission imply the presence of very large magnetic structures. Conceivable scenarii are a) θ¹ Orionis A2 is a single young intermediate-mass star with strong magnetic interactions between the star and its circumstellar disk, b) θ^1 Orionis A2 is a binary and radio flaring originates from interactions between the magnetic structures of both stars.