Mixing of Clumpy Supernova Ejecta into Molecular Clouds
  Several lines of evidence, from isotopic analyses of meteorites to studies of the Sun's elemental and isotopic composition, indicate that the solar system was contaminated early in its evolution by ejecta from a nearby supernova (SN). Previous models have invoked SN material being injected into an extant protoplanetary disk, or isotropically expanding ejecta sweeping over a distant (>10 pc) cloud core, simultaneously enriching it and triggering its collapse. Here we consider a new astrophysical setting: the injection of clumpy SN ejecta, as observed in the Cas A SN remnant, into the molecular gas at the periphery of an HII region created by the SN's progenitor star. To track these interactions we have conducted a suite of high-resolution (1500^3 effective) 3D simulations that follow the evolution of individual clumps as they move into molecular gas. Even at these high resolutions, our simulations do not quite achieve numerical convergence, due to the challenge of properly resolving the small-scale mixing of ejecta and molecular gas, although they do allow some robust conclusions to be drawn. Isotropically exploding ejecta do not penetrate into the molecular cloud, but, if cooling is properly accounted for, clumpy ejecta penetrate to distances ~10^18 cm and mix effectively with star-forming molecular gas. The ~2 M_\odot high-metallicity ejecta from a core-collapse SN is likely to mix with ~2 \times 10^4 M_\odot of molecular gas. Thus all stars forming late (~5 Myr) in the evolution of an HII region may be contaminated by SN ejecta at a level ~10^-4. This level of contamination is consistent with the abundances of short-lived radionuclides and possibly some stable isotopic shifts in the early solar system, and is potentially consistent with the observed variability in stellar elemental abundances. SN contamination of forming planetary systems may be a common, universal process. 
Liubin Pan, Steven J. Desch, Evan Scannapieco, and F. X. Timmes
astro-ph.SR astro-ph.EP