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A key test of the supernova triggering and injection hypothesis for theorigin of the solar system's short-lived radioisotopes is to reproduce theinferred initial abundances of these isotopes. We present here the mostdetailed models to date of the shock wave triggering and injection process,where shock waves with varied properties strike fully three dimensional,rotating, dense cloud cores. The models are calculated with the FLASH adaptivemesh hydrodynamics code. Three different outcomes can result: triggeredcollapse leading to fragmentation into a multiple protostar system; triggeredcollapse leading to a single protostar embedded in a protostellar disk; orfailure to undergo dynamic collapse. Shock wave material is injected into thecollapsing clouds through Rayleigh-Taylor fingers, resulting in initiallyinhomogeneous distributions in the protostars and protostellar disks. Cloudrotation about an axis aligned with the shock propagation direction does notincrease the injection efficiency appreciably, as the shock parameters werechosen to be optimal for injection even in the absence of rotation. For a shockwave from a core-collapse supernova, the dilution factors for supernovamaterial are in the range of $\sim 10^{-4}$ to $\sim 3 \times 10^{-4}$, inagreement with recent laboratory estimates of the required amount of dilutionfor $^{60}$Fe and $^{26}$Al. We conclude that a type II supernova remains as apromising candidate for synthesizing the solar system's short-livedradioisotopes shortly before their injection into the presolar cloud core bythe supernova's remnant shock wave.

astrophysical journal/the astrophysical journal

Triggering Collapse of the Presolar Dense Cloud Core and Injecting  Short-Lived Radioisotopes with a Shock Wave. III. Rotating Three Dimensional  Cloud Cores