Cococubed.com Piecewise Parabolic Method (PPM)
Home Astronomy research 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 Presentations Illustrations cococubed YouTube Bicycle adventures Public Outreach Education materials 2023 ASU Solar Systems Astronomy 2023 ASU Energy in Everyday Life AAS Journals AAS YouTube 2023 MESA VI 2023 MESA Marketplace 2023 MESA Classroom 2022 Earendel, A Highly Magnified Star 2022 White Dwarfs & 12C(α,γ)16O 2022 Black Hole Mass Spectrum 2022 MESA in Don't Look Up 2021 Bill Paxton, Tinsley Prize Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	The tool ppm.tbz is a simplified 1D PPM hydrodynamics solver on Cartesian grids. This tool is originally from Bruce Fryxell. While the Sod problem has become a standard hydrodynamic test case, it isn't a very discriminating test for modern software instruments. The strong shock tube problem below is more demanding because of the stronger discontinuities across the shock interface and the narrow density peak that forms behind the shock. The γ=1.4 test case sets the initial density to $\rho =10$ for $x < 2$, $\rho = 1$ for $x > 2$, and the initial pressure to $P =100$ for $x < 2$, $P = 1$ for $x > 2$. Below, the PPM solution and the exact solution to the exact Riemann solution at 0.4 s are compared. For a reasonably modern hydrodynamics software instrument with more capabilities (e.g., a more general equation of state or nuclear reaction networks, check out FLASH. Mike Zingale's codes page offers several lovely open-source hydrodynamic tools for research and teaching. Also see Mike's Zingale's hydro1d github project. For open, modern, multi-physics, multi-scale, and multi-dimensional hydrodynamic instruments, check out CASTRO, MAESTO, PHANTOM, and DEDALUS.
	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.