Authors: K. Katarzyński
Journal: Transactions of IAA RAS vol. 40
Keywords: VLBI, Exoplanets, Astrometry
We estimate possible radio emission of massive exoplanets and brown dwarfs. We assume that such radiation originates in processes similar to those observed in the Jupiter system. Therefore, we analyse two possible emission scenarios. The first scenario assumes interaction between the stellar wind and the planetary magnetosphere. The second mechanism needs a moon orbiting close to the planet, and is similar to the Jupiter-Io interaction. We show that the emission of exoplanets and brown dwarfs, in young systems (age < 0.1 Gyr) can be observed even at GHz frequencies. Therefore, VLBI networks could possibly detect such radiation. Moreover, an excellent angular resolution of VLBI should also allow to observe orbital movement in nearby (distance < 30 pc) systems.