*
Cococubed.com


Nuclear Reaction Networks

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.
Integration of Nuclear Reaction Networks for Stellar Hydrodynamics (2000)

In this article, methods for solving the stiff system of ordinary differential equations that constitute nuclear reaction networks are surveyed. Three semi-implicit time integration algorithms are examined; a traditional first-order-accurate Euler method, a fourth-order-accurate Kaps-Rentrop method, and a variable-order Bader-Deuflhard method. These three integration methods are coupled to eight different linear algebra packages. Four of the linear algebra packages operate on dense matrices (LAPACK, LUDCMP, LEQS, GIFT), three of them are designed for the direct solution of sparse matrices (MA28, UMFPACK, Y12M), and one uses an iterative method for sparse matrices (BiCG). The scaling properties and behavior of the 24 combinations (3 time integration methods times 8 linear algebra packages) are analyzed by running each combination on seven different nuclear reaction networks.

These reaction networks range from a hardwired 13 isotope $\alpha$-chain and heavy-ion reaction network, which is suitable for most multidimensional simulations of stellar phenomena, to a 489 isotope reaction network, which is suitable for determining the yields of isotopes lighter than technetium in spherically symmetric models of Type II supernovae. Each of the time integration methods and linear algebra packages are capable of generating accurate results, but the efficiency of the various methods -- evaluated across several different machine architectures and compiler options -- differ dramatically. If the execution speed of reaction networks that contain less than about 50 isotopes is an overriding concern, then the variable-order Bader-Deuflhard time integration method coupled with routines generated from the GIFT matrix package or LAPACK with vendor-optimized BLAS routines is a good choice. If the amount of storage needed for any reaction network is a concern, then any of the sparse matrix packages will reduce the storage costs by 70%-90%. When a balance between accuracy, overall efficiency, and ease of use is desirable, then the variable-order Bader-Deuflhard time integration method coupled with the MA28 sparse matrix package is a strong choice.


image
image
Kaps-Rentrop CPU time
image
Bader-Deuflard CPU time



An Inexpensive Nuclear Energy Generation Network for Stellar Hydrodynamics (2000)

In this article, we compare the nuclear energy generation rate and abundance levels given by an $\alpha$-chain nuclear reaction network that contains only seven isotopes with a standard 13 isotope α-chain reaction network. The energy generation rate of these two small networks are also compared to the energy generation rate given by a 489 isotope reaction network with weak reactions turned on and off. The comparison between the seven isotope and α-chain reaction networks indicate the extent to which one can be replaced by the other, and the comparison with the 489 isotope reaction network roughly indicates under what physical conditions it is safe to use the seven isotope and $\alpha$-chain reaction networks.

The seven isotope reaction network reproduces the nuclear energy generation rate of the standard $\alpha$-chain reaction network to within 30%, but often much better, during hydrostatic and explosive helium, carbon, and oxygen burning. It will also provide energy generation rates within 30% of an $\alpha$-chain reaction network for silicon burning at densities less than 10$^{7}$ g cm$^{-3}$. Provided there remains an equal number of protons and neutrons (Y$_e$ = 0.5) over the course of the evolution, and that flows through $\alpha$ particle channels dominate, then both of the small reaction networks return energy generation rates that are compatible with the energy generation rate returned by the 489 reaction network. If Y$_e$ is significantly different from 0.5, or if there are substantial flows through neutron and protons channels, then it is not generally safe to employ any $\alpha$-chain based reaction network. The relative accuracy of the 7 isotope reaction network, combined with its reduction in the computational cost, suggest that it is a suitable replacement for $\alpha$-chain reaction networks for parameter space surveys of a wide class of multidimensional stellar models.


image
Energy generation rate comparision
image
Ratio of energy generation rates
image
Isotope evolution



Nuclear Reaction Network Software Instruments

Open source software instruments are avaliable here.