Core Collapse Supernova Thermodynamics


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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.