Cococubed.com Mixing of Supernova Ejecta
Home Astronomy research   Software Infrastructure:      MESA      FLASH      STARLIB      MESA-Web      starkiller-astro      My instruments   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:      Neutrino HR diagram      Pulsating white dwarfs      Pop III with JWST      Monte Carlo massive stars      Neutrinos from pre-SN      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:      Iron Pseudocarbynes      Radionuclides in the 2020s      Hypatia catalog      Zone models H to Zn      Mixing ejecta      γ-rays within 100 Mpc   Thermodynamics & Networks      Stellar EOS      12C(α,γ)16O Rate      Proton-rich NSE      Reaction networks      Bayesian reaction rates   Verification Problems:      Validating an astro code      Su-Olson      Cog8      Mader      RMTV      Sedov      Noh Software instruments Presentations Illustrations cococubed YouTube Bicycle adventures Public Outreach Education materials AAS Journals AAS YouTube 2020 Celebration of Margaret Burbidge 2020 Digital Infrastructure 2021 MESA Marketplace 2021 MESA Summer School 2021 ASU Solar Systems 2021 ASU Energy in Everyday Life Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	Mixing of Supernova Ejecta into Molecular Clouds (2012) 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. Previous models have invoked supernova material being injected into an extant protoplanetary disk, or isotropically expanding ejecta sweeping over a distant ($>$10 pc) cloud core, simultaneously enriching it and triggering its collapse. In this article, we consider a new astrophysical setting: the injection of clumpy supernova ejecta, as observed in the Cassiopeia A supernova remnant, into the molecular gas at the periphery of an H II region created by the supernova's progenitor star. To track these interactions, we have conducted a suite of high-resolution (1500$^3$ effective) three-dimensional numerical hydrodynamic 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 or mix with it, but, if cooling is properly accounted for, clumpy ejecta penetrate to distances $\simeq$ 10$^{18}$ cm and mix effectively with large regions of star-forming molecular gas. In fact, the $\simeq$ M$_{\odot}$ of high-metallicity ejecta from a single core-collapse supernova is likely to mix with $\simeq$ 2$\times$ 10$^4$ M$_{\odot}$ of molecular gas material as it is collapsing. Thus, all stars forming late ($\approx$ 5 Myr) n the evolution of an H II region may be contaminated by supernova ejecta at the level $\simeq$10$^{-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 Ejecta delivery distance Volume rendering of density evolution Gas density and concentration