

Home 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 FermiDirac functions Galactic chemical evolution Coating an ellipsoid Universal twobody 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 Phyllotaxis The pendulum Circular and elliptical 3 body MESA MESAWeb FLASH Zingale's software Brown's dStar GR1D code Iliadis' STARLIB database Herwig's NuGRID Meyer's NetNuc Presentations Illustrations cococubed and AAS Videos Bicycle adventures AAS Journals 2019 Digital Infrastructure 2019 JINA Rprocess 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. 
The electronpositron portion of the two equations of state are identical. Differences between the two EOS routines originate from the model used for nucleons (interacting nucleons in a liquid dropish model versus noninteracting Boltzmann nucleons), and the model used for the composition. LS Baryon Pressure:
In certain regions of the rhoT plane, contributions from the coulomb lattice terms cause the baryon pressure to become negative. LS Total Pressure:
NSE Baryon Pressure:
Even though the nuclei in the NSEbased model are a perfect gas, the surface isn't planar because of the changing composition. This causes the ripples in the surface. NSE Total Pressure:
LS and NSE Pressures Compared:



