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K. W. Davis, M. D. Leising (Clemson University)
Live short-lived radionuclides detected in early solar system materials constrain the time between their creation and the formation of solids in the early solar system. The travel time from a stellar source and time for the presolar cloud to start condensing into solids would seem to take too long for radionuclides with lifetimes of only a few Myr to still be alive. Among several possible explanations is a supernova explosion near the presolar cloud both seeding the cloud with the short-lived radionuclides and initiating cloud collapse. Several of the detected short-lived radionuclides are only found deep within the supernova material, begging the question of how they become incorporated into a molecular cloud when the ISM and outer layers of ejecta lie between them and the cloud. Some have proposed that hydrodynamic instabilities can inject the appropriate material into the cloud. We perform simulations using the Zeus-2D hydrodynamic code to investigate the effect of hydrodynamic instabilites on injection of supernova material into a cold molecular cloud. We model the supernova as a hot, high density bubble of gas allowed to expand into the ISM and collide with a cold dense cloud and give it a very low value of angular momentum to distiguish its material from the ambiant ISM and cloud material.
The author(s) of this abstract have provided an email address for comments about the abstract: kwdavis@clemson.edu
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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.