Disk wind

The central star or protostar or the accretion process is emitting high-energy photons, from far-ultraviolet to x-rays.

One important function of the MHD wind is that it transports angular momentum away from the disk and the protostar.

[5] Studies have shown that disk wind is the major contributor to accretion in young stellar objects.

The reduced density of the inner disk can slow down, prevent or reverse planet migration in this region.

[5] But JWST has already contributed to the discovery of multiple resolved molecular disk winds.

[12] Outflows around supermassive black holes (SMBH) can be classified as either fast and collimated jets, or as slow (≤20% speed of light), but more massive disk winds.

In this scenario UV photons, which are produced in the disk near the SMBH, are scattered by strong resonance lines.