Core Collapse Supernova Thermodynamics


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
   Hotter white dwarfs

   Cold neutron stars
   Stellar opacities
   Neutrino energy loss rates
   Ephemeris routines
   Fermi-Dirac functions

   Galactic chemical evolution
   Coating an ellipsoid
   Universal two-body problem

   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
   Verification problems
   Plane - cube Intersection

   The pendulum
   Circular and elliptical 3 body


   Zingale's software
   Brown's dStar
   GR1D code
   Iliadis' STARLIB database
   Herwig's NuGRID
   Meyer's NetNuc
Bicycle adventures

AAS Journals
2019 JINA R-process Workshop
2019 MESA Marketplace
2019 MESA Summer School
2019 AST111 Earned Admission
Teaching materials
Education and Public Outreach

Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.

Background material:
Click here If you want to brush up on NSE calculations, or here if you want a refresher on stellar EOS calculations, or here if you want the Lattimer-Swesty nuclear EOS. A testing routine for the Lattimer-Swesty EOS. Hooks for calling any electron-positron thermodynamics routine, not just the one included in the LS package.

Comparison of the NSE and LS neutron, proton, alpha particle and heavy nucleus mass fractions, and the mean charge Zbar of the heavy nucleus.

Pressure and its derivatives with temperature and density.
Energy and its derivatives with temperature and density.
Entropy and its derivatives with temperature and density.
for an NSE and the LS approachs.

Effect On Core Collapse Models:
Preliminary results model suggest if the NSE state is a boundary condition for the LS EOS to achieve as it falls out of the regime where nuclei are strongly coupled, it misses by a bit. These sn models, suggest what may happen in some Type II supernova models if one uses the LS everywhere (even in regimes where its authors say it shouldn't be used) versus using LS where appropriate and an NSE appraoch elsewhere. These preliminary results suggest models that employ LS everywhere get weaker convection (a shallower, less extensive, entropy gradient) while LS + NSE approaches get more vigorous convection over a larger region.
Conditions of interest

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.