Cococubed.com Mixing of Supernova Ejecta
Home Astronomy research   Software Infrastructure:      MESA      FLASH      STARLIB      My codes   White dwarf supernova:      Remnant metallicities      Colliding white dwarfs      Merging white dwarfs      Ignition conditions      Metallicity effects      Central density effects      Detonation density effects      Tracer particle burning      Subsonic burning fronts      Supersonic burning fronts      W7 profiles   Massive star supernova:      Rotating progenitors      3D evolution      26Al & 60Fe      44Ti, 60Co & 56Ni      Yields of radionuclides      Effects of 12C +12C      SN 1987A light curve      Constraints on Ni/Fe ratios      An r-process      Compact object IMF   Stars:      Pop III JWST      Pre-SN variations      Monte Carlo white dwarfs      SAGB stars      Classical novae      He shell convection      Presolar grains      He burn on neutron stars      BBFH at 40 years   Chemical Evolution:      Hypatia catalog      Zone models H to Zn      Mixing ejecta      γ-rays within 100 Mpc   Thermodynamics & Networks      Stellar EOS      Reaction networks      Proton-rich NSE      Bayesian reaction rates   Verification Problems:      Validating an astro code      Su-Olson      Cog8      Mader      RMTV      Sedov      Noh Software instruments Presentations Illustrations Videos Bicycle adventures AAS Journals 2017 MESA Marketplace 2017 MESA Summer School 2017 ASU+EdX AST111x Teaching materials Education and Public Outreach Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	Mixing of Supernova Ejecta into Molecular Clouds (2012) In this paper by Pan et al, we have conduct of high-resolution 3D numerical hydrodynamic simulations that follow the evolution of a single clump of supernova ejecta as it moves into molecular gas. Isotropically exploding ejecta do not penetrate into the molecular cloud or mix with it, but, if cooling is properly accounted for, clumpy ejecta penetrate to distances 1018 cm} and mix effectively with large regions of star-forming molecular gas. In fact, the 2 M⊙ of high-metallicity ejecta from a single core-collapse supernova is likely to mix with 3×104 M⊙ of molecular gas material as it is collapsing. Thus all stars forming late (5 Myr) in the evolution of an H II region may be contaminated by supernova ejecta at the 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. Supernova contamination of forming planetary systems may be a common, universal process. Cooling timescales Gas density and concentration Volume rendering of density evolution Ejecta delivery distance