The Internal Constitution of the StarsCambridge University Press, 28 янв. 1988 г. - Всего страниц: 407 The publication of The Internal Constitution of the Stars by Arthur Eddington in 1926 was a major landmark in the development of modern theoretical astrophysics. Not only did Eddington effectively create the discipline of the structure, constitution, and the evolution of the stars, but he also recognised and established the basic elements of our present understanding of the subject. The influence of the book is indicated by the remark by H. N. Russell in 1945: 'This volume has every claim to be regarded as a masterpiece of the first rank'. |
Содержание
Survey of the Problem | 1 |
Thermodynamics of Radiation | 27 |
Quantum Theory | 44 |
Polytropic Gas Spheres | 79 |
Radiative Equilibrium | 97 |
Solution of the Equations | 114 |
A Central Temperature and Mean Density for given Mass | 120 |
The MassLuminosity Relation | 145 |
Ionisation Diffusion Rotation | 250 |
38 | 266 |
The Source of Stellar Energy | 289 |
The Outside of a Star | 321 |
Values of Ratio of Specific Heats for Stellar Material | 370 |
Diffuse Matter in Space | 371 |
Physical and Astronomical Constants | 395 |
References | 397 |
Data for Stars on the Main Series Central Temperature | 178 |
Variable Stars | 180 |
The Coefficient of Opacity | 216 |
| 403 | |
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absolute magnitude absorbed absorption coefficient according approximation astronomical atoms average bolometric magnitude brightness calcium calculated Capella capture central temperature centre Cepheids chromosphere column component considered constant corresponding curve determined deviation diffuse diffuse nebulae distribution dwarf E. A. MILNE effective temperature elements emission emitted equation equilibrium ergs excited factor formula free electrons frequency giant stars given gives heat Hence hydrogen hypothesis increase integral intensity interior interstellar ionisation ions Kramers limit luminosity M₁ main series mass material matter maximum mean molecular weight molecules momentum Monthly Notices nebulae nucleus observed obtain opacity orbits P₁ parallax parsecs perfect gas photosphere potential proportional pulsation quantum radiation pressure radius range ratio region rotation spectral type spectrum stellar subatomic energy suppose surface T₁ Table terrestrial theory thermodynamical thermodynamical equilibrium tion variables velocity visual magnitude wave-length