Hydrodynamics of Radioactivity Injection into the Presolar Cloud

Details Hydrodynamics of Radioactivity Injection into the Presolar Cloud Hydrodynamics of Radioactivity Injection into the Presolar Cloud

Nov 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..ses.jb007d&link_type=abstract

American Physical Society, The 70th Annual Meeting of the Southeastern Section, November 6-8, 2003, Wilmington, North Carolina,

Physics

Scientific paper

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 time for travel from a stellar source and condensation of solids in the presolar cloud would seem to be 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 it with the short-lived radionuclides and initiating cloud collapse. Several of the detected short-lived radionuclides are only found deep within the supernova material, raising the question of how their incorporation into a molecular cloud occurs when the interstellar medium and outer layers of the exploded star lie between them. We present the latest results of two-dimensional hydrodynamical simulations modeling this scenario.

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