

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 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 MESA MESAWeb FLASH Zingale's software Brown's dStar GR1D code Iliadis' STARLIB database Herwig's NuGRID Meyer's NetNuc Presentations Illustrations Videos Bicycle adventures AAS Journals 2017 MESA Summer School ASU+EdX AST111x Teaching materials Education and Public Outreach 2016 NSF SI2 PI Workshop Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement. 
The code contained in public_poly.tbz computes the structure of stars that are in hydrostatic equilibrium and obey a polytropic equation of state. The code solves the dimensionless LaneEmden equation and writes out a solution in physical units. Certain polytropic stars are related cold white dwarfs.



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 coauthorship as appropriate. 
