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It has been suggested in the past that at least part of the emission observed in high-velocity outflows from young stars could be formed in turbulent mixing layers. A simplified mixing layer model based on a simple 'turbulent viscosity' description of the dissipation and transport associated with the fully developed turbulence. Predictions from these models agree very well with results from laboratory flows with Mach numbers M = 1 to 20, showing that this theoretical approach is indeed valid for the M about 10 regime that is relevant for stellar outflows. Mixing layers have a sizeable radiative luminosity, so that in principle they could substantially contribute to the total emission from stellar jets or from Herbig-Haro objects. The theoretical framework presented is quite general, and could be applied to mixing layers with detailed atomic and/or molecular processes (as would be necessary for modeling molecular outflows), or to mixing layers with different geometries (e.g., the accretion disk/stellar photosphere boundary layer).
Cantó et al. (1991) studied this question.