Statistics – Computation
Scientific paper
May 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...372..646c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 372, May 10, 1991, p. 646-658. Research supported by Universidad Nacional A
Statistics
Computation
130
Early Stars, Mixing Layers (Fluids), Stellar Envelopes, Stellar Mass Ejection, Computational Astrophysics, Emission Spectra, Herbig-Haro Objects, Jet Flow
Scientific paper
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 Jorge
Raga Alejandro C.
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