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| Core Collapse Supernova Thermodynamics |
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Background material:
Click here If you need to brush up on NSE calculations, or here if you need a refresher on "normal" stellar EOS calculations, or here if you need to get the Lattimer-Swesty nuclear EOS.
A testing routine for the Lattimer-Swesty EOS. In this version I include the hooks for calling any electron-positron thermodynamics routine, not just the one included in the LS package.
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Composition: These pages show and compare the compositions of an NSE approach and the LS approach, in particular the, neutron, proton, alpha particle, and representative heavy nucleus mass fractions. The composition of the representative heavy nucleus is shown here. Thermodynamics: 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. |
Conditions of interest |
Some of the protaganists in this passion play met at LANL in December 2002. Some preliminary results generated at the meeting are shown here. The bottom line appears to be that if one thinks of the NSE state as a boundary condition for the LS EOS to achieve as it falls out of the regime where nuclei are strongly coupled, well ... it misses it by a bit.
These models, generated for the most part at the meeting, illustrates 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 its appropriate and an NSE appraoch elsewhere. The bottom line seems to be that 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.