We present theoretical predictions for the free–free emission at centimeter wavelengths obtained from photoevaporation and magnetohydrodynamic (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 the Atacama Large Millimeter/submillimeter Array. 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 Next Generation Very Large Array would have enough sensitivity and angular resolution to spatially resolve the main structures predicted by these models.

我们提出了从光蒸发和磁流体动力学 (MHD) 风盘模型中获得的厘米波长自由发射的理论预测，这些模型根据 TW Hydrae 年轻恒星物体的情况进行了调整。对于该系统，由于来自恒星的高能光子加热，盘状光蒸发已被提议作为打开阿塔卡马大型毫米/亚毫米阵列尘埃发射中观察到的间隙的一种可能机制。我们表明光蒸发盘模型预测了自由发射的径向剖面，它由两个主要空间分量组成，一个来自距离恒星 0.5-1 au 的束缚盘大气，另一个来自光蒸发的更扩展分量。以更大的圆盘半径风。我们还表明，恒星 X 射线光度对这两个分量都有显着影响。来自 MHD 风模型的预测射电辐射具有更平滑的径向分布，与光蒸发情况相比，它延伸到离恒星更近的距离。我们还表明，未来的射电望远镜，例如下一代超大阵列，将具有足够的灵敏度和角分辨率，可以在空间上解析这些模型预测的主要结构。