*
Cococubed.com


Cold White Dwarfs

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
   Fermi-Dirac functions

   Galactic chemical evolution
   Coating an ellipsoid

   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

   MESA
   MESA-Web
   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 Marketplace
2017 MESA Summer School
2017 ASU+EdX AST111x
Teaching materials
Education and Public Outreach


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

The tool in public_coldwd.tbz can generate models of general relativistic corrected white dwarfs in hydrostatic equilibrium. A cold, perfectly degenerate, electron gas equation of state \begin{equation} \begin{split} x & = \left [ \dfrac{3}{8 \pi} \left ( \dfrac{h}{m_ec}\right )^3 N_A Y_e \rho \right ]^{1/3} \\ f(x) & = x (x^2 + 1)^{1/2}(2x^2 - 3) + 3\ln(x + (x^2 + 1)^{1/2}) \\ g(x) & = 8x^3 \left [ (x^2 + 1)^{1/2} -1) \right ] - f(x) \\ P_e & = \dfrac{\pi m_e^4 c^5}{3 h^3} \cdot f(x) \hskip 1.0in E_e = \dfrac{\pi m_e^4 c^5}{3 h^3} \cdot g(x) \end{split} \label{eq1} \tag{1} \end{equation} is included. The code is presently set to generate the central density - mass plot below. Uncommenting a few lines will generate the last two plots. A quote from Icko circa 1985 about generating white dwarf models comes to mind ...


image
Central Density - Mass relation
image
Density profiles
image
Mass-radius relation


 



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.