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K. W. Davis, M. D. Leising (Clemson University)
Short-lived radionuclides (RNs) such as 60Fe, 53Mn, and 41Ca, with half-lives of 1.5, 3.7, and 0.1 Myr, respectively, have been detected as present and live in the early phases of the solar system's formation. To date, roughly 10 isotopes with half-lives less than 103 Myr have been detected or are suggested as being present in the early solar system. The times to transport these radionuclides to the solar system formation site and the free fall time of the presolar cloud is far longer than their mean lifetimes and excludes the steady state interstellar abundance as an appropriate model for the source of these radionuclides. Several of these nuclides are produced almost exclusively in Supernovae (SNe). The hypothesis that a SN event near the formation site of the solar system both provided the radioactive materials to the progenitor cloud and caused rapid collapse of the pre-solar cloud has been well-studied. However, previous work by other authors has modeled the interaction of the shock, which is well ahead of the ejecta, and a hypothetical presolar cloud, but has not explicitly modeled the origin of the material that becomes incorporated into the cloud. Several of the RNs in question are produced near the core of the SN. To explain their existence in the early solar system, the material in question must make it through the overlying material of the SN progenitor, through any mass lost by the progenitor before explosion, and through the intervening ISM to reach the presolar cloud. Using Zeus-2D, a general hydrodynamics code developed for studying astrophysical phenomena, this work will expand upon previous studies by presenting interactions between a SN shockwave and a stationary cloud, explicitly tracking material from the explosion to the cloud. We explore several assumptions of adiabaticity and the effect of simple models of cooling on our calculations.
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.