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Recent meteoritical analyses support an initial abundance of the short-livedradioisotope $^{60}$Fe that may be high enough to require nucleosynthesis in acore collapse supernova, followed by rapid incorporation into primitivemeteoritical components, rather than a scenario where such isotopes wereinherited from a well-mixed region of a giant molecular cloud polluted by avariety of supernovae remnants and massive star winds. This paper continues toexplore the former scenario, by calculating three dimensional, adaptive meshrefinement, hydrodynamical code (FLASH 2.5) models of the self-gravitational,dynamical collapse of a molecular cloud core that has been struck by a thinshock front with a speed of 40 km/sec, leading to the injection of shock frontmatter into the collapsing cloud through the formation of Rayleigh-Taylorfingers at the shock-cloud intersection. These models extend the previous workinto the nonisothermal collapse regime using a polytropic approximation torepresent compressional heating in the optically thick protostar. The modelsshow that the injection efficiencies of shock front material are enhancedcompared to previous models, which were not carried into the nonisothermalregime and so did not reach such high densities. The new models, combined withthe recent estimates of initial $^{60}$Fe abundances, imply that the supernovatriggering and injection scenario remains as a plausible explanation for theorigin of the short-lived radioisotopes involved in the formation of our solarsystem.

Triggering Collapse of the Presolar Dense Cloud Core and Injecting Short-Lived Radioisotopes with a Shock Wave. V. Nonisothermal Collapse Regime