As a quantitative example of how relatively complex astrophysical
phenomena
can be explored with ease using APL, we have developed a structure
model
for white dwarf stars. The model presented here considers such
effects
as Coulomb interactions between electrons and nucleons, inverse beta
decays,
and the effects of the general theory of relativity on the condition of
hydrostatic equilibrium. This structure model is valid for
zero-temperature
stars of varying chemical compositions, ionic partitions, and central
densities;
and is applicable over a wide range of partial and total degeneracy
regimes.
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ACM Portal for Conference: Here
VIEGRAPHS from Presentation:
1. Functional Layering
2. Structure Equations
3. Equation of State
4. Equation of State (continued)
5. Structure Equtions in APL
6. Relativity Parameter
7. Numerical Integration
8. WHITEDWARF model
9. Structure: P/r
10. Structure: m/r
11. Mass vs. Radius
12. Stellar Rotation
13. Uniform Rotation
14. Figures of Equilibrium
15. Rotational Instability
16. Break Up Rotation
