内容

目次

I. General Considerations Concerning the Energy Radiated by Stars.- 1. The Energy Output and Its ‘Spectral Composition’.- 2. The Observational Data.- 3. Generalities Concerning the Energy Sources.- II. Mechanical Equilibrium: The Equilibrium between the Gravitational Force Per Unit Volume and the Gradient of the Total Pressure.- 1. Introduction.- 2. The Equilibrium between the Gradient of the Total Pressure and the Gravitational Force per Unit Volume.- 2.1. Newton’s Theorem. The Gravitational Force per Unit Volume.- 2.2. The Force per Unit Volume Produced by the Pressure Gradient.- 2.3. The Equation Expressing the Mechanical Equilibrium of (dV).- 3. The Relation between Mrand the Density ? at a Distance r from the Center.- 4. The Expression for div g as a Function of the Local Density ?. Poisson’s Equation.- 5. The Calculation of the Gas Pressure Pgas. The Concept of the Mean Mass µ of a Particle of the Mixture in Units of mH (where mHis the Mass in Grams of a ‘Real’ Microscopic Hydrogen Atom).- 6. A Model of the Sun at ‘Constant Density’ ? = ??.- 7. The ‘Homologous’ Model. Expressions for Pc and Tcin Terms of M and R.- Exercises.- III. The Determination of the Internal Structure by the Density Distribution ?(r).- 1. Introduction.- 2. The Determination of the Distribution of the Mass Mr Contained in a Sphere of Radius r.- 3. The Determination of the Distribution of the Total Pressure P as a Function of r.- 4. The Determination of the Distribution of the Temperature T as a Function of r.- 5. Summary. The Empirical Representation of the Functions g (r’),?(r’), P(r’), and T(r’). The Polytropic Index n.- 6. The (Superficial) ‘Convective Zone’ of the Sun.- Exercises.- IV. Energy Equilibrium and Nuclear Reactions.- 1. The Equation of Energy Equilibrium.- 2. The p-p Chain and the C-N Cycle.- 2.1. Introduction.- 2.2. An Explicit Schematic Representation of the Composition of Nuclei.- 2.3. The Details of the Reactions in the p-p Chain (Bethe, 1938).- 2.4. The Details of the C-N Cycle (Bethe, 1938).- 3. Calculation of the Energy ?. Generalities.- 3.1. Calculation of R12 for a Given Reaction.- 4. The ‘Mean Lifetime’ of a Given Nucleus with Respect to an Isolated Reaction (R).- 4.1. Generalities.- 4.2. The Physical Meaning of ?p(c).- 4.3. ?p(c)as the ‘Mean Duration of an Isolated Reaction (R)’.- 4.4. ?p(c)as an ‘Exponential Decrement’.- 4.5. The Transition Probability pcaper Reaction (R).- 5. The Convergence of Cyclic Reactions to a Stationary (‘Equilibrium’) State.- 6. The ‘Mean Duration of a Cycle’. The Calculation of the Energy ? when Cyclic Reactions Are Present.- 7. The Empirical Representation of ?pp and ?CN.- 8. Application to the Sun. The ‘Final Test’.- 8.1. Review of the Principal Results.- 8.2. The Region in which ?Is Negligible.- 8.3. The ‘Central’ Region (r’< 0.40), where L’rand X Vary.- 8.4. The ‘Final Test’.- Exercises.- V. Evolutionary Models. The Actual Determination of Structure.- 1. Introduction.- 1.1. The Advantage of Studying ‘Evolutionary Sequences’.- 1.2. The ‘Fossilized’ Composition.- 2. The Evolution of the Distributions X(r)and Y(r).- 3. Discussion.- 4. The Mathematical Structure of the Problem. Principles of the Integration Methods.- 5. The Age of a Star.- 6. The Relations between P, T, L, R, and Parameters such as M, k0, ?0, and µ for ‘Homologous’ Models. The ‘Mass-Luminosity’ and ‘Mass-Radius’ Relations.- Conclusion.- Solutions for the Exercises.- Index of Subjects.