Testing photoevaporation and MHD disk wind models through future high-angular resolution radio observations: the case of TW Hydrae

TL;DR

This paper compares photoevaporation and MHD wind models for TW Hydrae, predicting their radio emission profiles and assessing the capabilities of future radio telescopes like ngVLA to resolve these structures.

Contribution

It provides detailed theoretical predictions of free-free emission from both models tailored to TW Hydrae, highlighting differences in spatial distribution and the impact of stellar X-ray luminosity.

Findings

Photoevaporation model predicts two main emission components at different radii.

MHD wind model shows a smoother, more extended emission profile.

Future ngVLA observations can spatially resolve these predicted structures.

Abstract

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.