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Fundamentals of equations of state /
The equation of state was originally developed for ideal gases, and proved central to the development of early molecular and atomic physics. Increasingly sophisticated equations of state have been developed to take into account molecular interactions, quantization, relativistic effects, etc. Extreme...
| Clasificación: | Libro Electrónico |
|---|---|
| Autor principal: | |
| Otros Autores: | , |
| Formato: | Electrónico eBook |
| Idioma: | Inglés |
| Publicado: |
River Edge, N.J. :
World Scientific,
©2002.
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| Temas: | |
| Acceso en línea: | Texto completo |
Tabla de Contenidos:
- 1. Introduction. 1.1. General remarks. 1.2. Phenomena at various densities and temperatures. 1.3. Quantum pressure and compressibility. 1.4. Pressure-temperature diagram. 1.5. Radiation effects
- 2. A summary of thermodynamics. 2.1. Phenomenology. 2.2. Statistical picture. 2.3. Maxwell-Boltzmann distribution
- 3. Equation of state for an ideal gas. 3.1. The partition function. 3.2. Thermodynamic functions. 3.3. The Gibbs' paradox
- 4. Law of equipartition of energy and effects of vibrational and rotational motions. 4.1. Classical considerations. 4.2. The partition function. 4.3. The vibrational partition function. 4.4. The rotational partition function. 4.5. The electronic partition function. 4.6. Summary
- 5. Bose-Einstein equation of state. 5.1. Introduction. 5.2. Classical statistics. 5.3. Bose-Einstein statistics without restriction on the total number of particles: photons. 5.4. Bose-Einstein statistics for a constant number of particles
- 6. Fermi-Dirac equation of state. 6.1. Overview. 6.2. The grand partition function and other thermodynamic functions. 6.3. Relativistic considerations. 6.4. Adiabatic processes
- 7. Ionization equilibrium and the Saha equation. 7.1. Introduction. 7.2. The thermodynamic formulation. 7.3. The Saha ionisation formula
- 8. Debye-Huckel equation of state. 8.1. Introduction. 8.2. Charged particle description. 8.3. Electrostatic energy. 8.4. Total free energy and equation of state
- 9. The Thomas-Fermi and related models. 9.1. Overview. 9.2. The Thomas-Fermi model at T = 0. 9.3. Inclusion of exchange interaction: the Thomas-Fermi-Dirac equation. 9.4. Derivation of equation (9.103) using the virial theorem. 9.5. The Thomas-Fermi model at finite temperatures. 9.6. Exchange and quantum corrections to the Thomas-Fermi model
- 10. Gruneisen equation of state. 10.1. Introduction. 10.2. The Einstein model of solids. 10.3. The Debye model of solids. 10.4. The Gruneisen relation. 10.5. Slater-Landau calculation of [symbol]. 10.6. Results and discussion
- 11. An introduction to fluid mechanics in relation to shock waves. 11.1. Fluid equations of motion. 11.2. Sound waves and Rieman invariants. 11.3. Rarefaction waves. 11.4. Shock waves and the Hugoniot relation
- 12. Derivation of hydrodynamics from kinetic theory. 12.1. Foundations of hydromechanics. 12.2. Distribution functions and the Boltzmann equation. 12.3. Loss of information. 12.4. Derivation of macroscopic equations
- 13. Studies of the equations of state from high pressure shock waves in solids. 13.1. Introduction. 13.2. The Gruneisen coefficient [symbol](V) and an equation for the cold pressure Pc. 13.3. The specific volume V[symbol] of the 'zero point' and the initial conditions for the Pc equation. 13.4. Isentropic processes near the Hugoniot curve and the free surface velocity. 13.5. Equations of state for aluminum, copper and lead. 13.6. Semi-empirical interpolation equation of state
- 14. Equation of state and inertial confinement fusion. 14.1. Pellet fusion. 14.2. The limiting case of isentropic (shock-free) volume ignition (self-similarity model). 14.3. Central core ignition with minimized entropy production. 14.4. Alternative driving schemes: nonlinear force, cannon ball. 14.5. The two-temperature equation of state
- 15. Applications of equations of state in astrophysics. 15.1. Overview. 15.2. The equation of hydrostatic equilibrium. 15.3. Expressions for pressure and temperature inside a star. 15.4. Numerical estimates of Pc, [symbol] and [symbol] by assuming uniform density inside the star. 15.5. Some useful theorems. 15.6. The gravitational potential energy and the virial theorem. 15.7. Qualitative understanding of the evolution of a star. 15.8. The contribution due to radiation pressure. 15.9. The polytropic model. 15.10. The standard model. 15.11. The white dwarf stars
- 16. Equations of state in elementary particle physics. 16.1. Overview. 16.2. Hagedorn model of strong interactions.