Nuclear Reaction Networks


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


   Zingale's software
   Brown's dStar
   GR1D code
   Iliadis' STARLIB database
   Herwig's NuGRID
   Meyer's NetNuc
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Public Outreach
Education materials
2023 ASU Solar Systems Astronomy
2023 ASU Energy in Everyday Life

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2023 White Dwarfs & 12C(α,γ)16O
2022 Earendel, A Highly Magnified Star
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.

Before using these reaction networks you should probably glance at my method of madness, Raph Hix's & Brad Meyer's excellent article, Brad Meyer's annual review article, George Wallerstein's review of modern physics article, and this National Nuclear Physics Summer School lectures on reaction networks.

There is a certain irremovable complexity associated with stiff systems of ordinary differential equations $$ \dot {{\bf y}} = {\bf f} \ ({\bf y}) \label{eq1} \tag{1} $$ when the right hand side is a complicated function, the Jacobian matrix $\tilde{{\bf J}}$ is sparse, and one wants a high-quality time integration. The tools below use an analytical Jacobian, a variable-order Bader-Deuflhard integration method, and MA28 sparse linear algebra. The reaction network and thermodynamics are integrated simultaneously. That is, they are fully coupled. Hydrostatic, one-step, adiabatic expansion, self-heating at constant density, self-heating through constant pressure, and arbitrary thermodynamic histories are currently supported.

These reaction networks are a snapshot of my current research efforts. If you want to put these reaction networks in a stellar evolution or hydrodynamics software instrument, and/or you want the networks to execute as efficiently as possible, feel free to contact me.

Make H & He

* Big Bang
Burn hydrogen

* pp chains

* cno cycles

* pp + cno

* hotcno + rp

* pp+hotcno+rp

* 8 isotopes

* 7 isotopes

* 13 isotopes

* 19 isotopes

* 21 isotopes

* Full H + He

Eat neutrons

* s-process
General network

* torch


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.