The formation of interstellar jets

Details The formation of interstellar jets The formation of interstellar jets

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...202..256t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 202, no. 1-2, Aug. 1988, p. 256-266. NASA-supported research.

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Computational Astrophysics, Conical Flow, Interstellar Matter, Stellar Winds, Supersonic Jet Flow, Collimation, Convergence, Cooling, Flow Geometry, Mach Number, Radiative Heat Transfer, Shock Wave Propagation

Scientific paper

The formation of interstellar jets by convergence of supersonic conical flows and the further dynamical evolution of these jets are investigated theoretically by means of numerical simulations. The results are presented in extensive graphs and characterized in detail. Strong radiative cooling is shown to result in jets with Mach numbers 2.5-29 propagating to lengths 50-100 times their original widths, with condensation of swept-up interstellar matter at Mach 5 or greater. The characteristics of so-called molecular outflows are well reproduced by the simulations of low-Mach-number and quasi-adiabatic jets.

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