Numerical simulations of triggered star formation

Details Numerical simulations of triggered star formation Numerical simulations of triggered star formation

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1479v&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 479.

Computer Science

Star Formation, Digital Simulation, Supernova Remnants, Radioactive Isotopes, Gravitational Collapse, Molecular Clouds, Hydrogen, Carbon Monoxide, Fragments

Scientific paper

The shock mechanism generated by a supernova explosion is examined via the Smoothed Particle Hydrodynamics (SPH) method to investigate under what conditions the impact of an interstellar shock wave will cause a molecular cloud core to collapse. The critical point in determining whether the shock is strong enough to compress the core is whether the principal coolants, CO and H2, survive in the shock front. No evidence is found for shock flow material being mixed into the core in the cases leading to collapse. A sequence of images from a simulation run leading to the formation of two collapsing fragments is shown.

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