Cococubed.com Galactic Chemical Evolution
Home Astronomy Research    Radiative Opacity    2024 Neutrino Emission from Stars    2023 White Dwarfs & 12C(α,γ)16O    2023 MESA VI    2022 Earendel, A Highly Magnified Star    2022 Black Hole Mass Spectrum    2021 Skye Equation of State    2021 White Dwarf Pulsations & 22Ne    Software Instruments      Stellar equation of states      EOS with ionization      EOS for supernovae      Chemical potentials      Stellar atmospheres      Voigt Function      Jeans escape      Polytropic stars      Cold white dwarfs      Adiabatic white dwarfs      Cold neutron stars      Stellar opacities      Neutrino energy loss rates      Ephemeris routines      Fermi-Dirac functions      Polyhedra volume      Plane - cube intersection      Coating an ellipsoid      Nuclear reaction networks      Nuclear statistical equilibrium      Laminar deflagrations      CJ detonations      ZND detonations      Fitting to conic sections      Unusual linear algebra      Derivatives on uneven grids      Pentadiagonal solver      Quadratics, Cubics, Quartics      Supernova light curves      Exact Riemann solutions      1D PPM hydrodynamics      Hydrodynamic test cases      Galactic chemical evolution      Universal two-body problem      Circular and elliptical 3 body      The pendulum      Phyllotaxis      MESA      MESA-Web      FLASH      Zingale's software      Brown's dStar      GR1D code      Iliadis' STARLIB database      Herwig's NuGRID      Meyer's NetNuc AAS Journals    2024 AAS YouTube    2024 AAS Peer Review Workshops 2024 ASU Energy in Everyday Life 2024 MESA Classroom Outreach and Education Materials Other Stuff:    Bicycle Adventures    Illustrations    Presentations Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	"Zone models" of galactic chemical evolution usually assert the abundance $N$ of an isotope $i$ follows \begin{equation} \frac{dN_i}{dt} = \rm{death} \ - \ \rm {birth} \ + \ \rm {infall} \ + \ \rm {decay} \ . \label{eq1} \tag{1} \end{equation} The death term (representing supernovae, kilonovae, classical novae, etc) is a sum of retarded time birth terms (stars born yesterday die today) , giving rise to a system of integro-differential equations \begin{equation} \begin{split} \frac{dN_i}{dt} & = \int_{M_{lo}}^{M_{hi}} B(t - \tau(m)) \ \Psi(m) \ N_i (t-\tau(m)) \ dm \\ & - \ B(t) \ \frac{N_i}{N_{\rm{gas}}} + \ {\dot N}_{i,\rm{gas}} + \frac{N_i}{\tau_{1/2,i}} \qquad {\rm M}_{\odot} \ {\rm pc}^{-3} \ {\rm Gyr}^{-1} \ , \end{split} \label{eq2} \tag{2} \end{equation} where $B(t)$ is the birth rate, $\tau(m)$ is the stellar lifetime, $\Psi(m)$ is the initial mass function, $N_{\rm{gas}}$ is the total surface gas density, ${\dot N}_{i,\rm{gas}}$ is the mass accretion rate, and $\tau_{1/2,i}$ is the half-life of the isotope. The tool chem3.tbz solves this system of integro-differentials. The tool includes a plain text nucleosynthesis data file, which one can easily modify, that contains isotopic contributions from Type II supernovae (Woosley & Weaver 1995), low mass stars (Renzini & Voli 1986), six different Type Ia supernovae models, three different classical novae models, and Big Bang nucleosynthesis. Hydrogen Through Zinc The chemical evolution of 76 stable isotopes, from hydrogen to zinc, is presented in this article. A grid of 60 Type II supernova models of varying mass (11 ≤ M/M⊙ ≤ 40) and metallicity (0, 10-4, 0.01, 0.1, and 1 Z⊙), is coupled with a simple dynamical model for the Milky Way. The results are compared in detail with the inferred atmospheric abundances for stars with metallicities in the range -3.0 ≤ [Fe/H] ≤ 0.0 dex. Sampled 4.6 billion years ago at a distance of 8.5 kpc, we find a composition at the solar circle that is within a factor of two of the solar abundances:
	Please cite the relevant references if you publish a piece of work that use these codes, pieces of these codes, or modified versions of them. Offer co-authorship as appropriate.