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When a planet transits in front of its host star, a fraction of its light isblocked, decreasing the observed flux from the star. The same is expected tooccur when observing the stellar radio flux. However, at radio wavelengths, theplanet also radiates, depending on its temperature, and thus modifies thetransit depths. We explore this scenario simulating the radio lightcurves oftransits of hot-Jupiters, Kepler-17b and WASP-12b, around solar-like stars. Wecalculated the bremsstrahlung radio emission at 17, 100, and 400 GHz originatedfrom the star, considering a solar atmospheric model. The planetary radioemission was calculated modelling the planets in two scenarios: as a blackbodyor with a dense and hot extended atmosphere. In both cases the planet radiatesand contributes to the total radio flux. For a blackbody planet, the transitdepth is in the order of 2-4% and it is independent of the radio frequency.Hot-Jupiters planets with atmospheres appear bigger and brighter in radio, thushaving a larger contribution to the total flux of the system. Therefore, thetransit depths are larger than in the case of blackbody planets, reaching up to8% at 17 GHz. Also the transit depth is frequency-dependent. Moreover, thetransit caused by the planet passing behind the star is deeper than when theplanet transits in front of the star, being as large as 18% at 400GHz. In allcases, the contribution of the planetary radio emission to the observed flux isevident when the planet transits behind the star.

Planetary transits at radio wavelengths: secondary eclipses of hot Jupiter extended atmospheres