  We present theoretical predictions for the free-free emission at cm
wavelengths obtained from photoevaporation and MHD wind disk models adjusted to
the case of the TW Hydrae young stellar object. For this system, disk
photoevaporation with heating due to the high-energy photons from the star has
been proposed as a possible mechanism to open the gap observed in the dust
emission with ALMA. We show that the photoevaporation disk model predicts a
radial profile for the free-free emission that is made of two main spatial
components, one originated from the bound disk atmosphere at 0.5-1 au from the
star, and another more extended component from the photoevaporative wind at
larger disk radii. We also show that the stellar X-ray luminosity has a
significant impact on both these components. The predicted radio emission from
the MHD wind model has a smoother radial distribution which extends to closer
distances to the star than the photoevaporation case. We also show that a
future radio telescope such as the \textit{Next Generation Very Large Array}
(ngVLA) would have enough sensitivity and angular resolution to spatially
resolve the main structures predicted by these models.
