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An introduction to the study of stellar structure, by Subrahmanyan Chandrasekhar
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In this monograph a leading modern astrophysicist explores a problem basic to stellar dynamics: What is the relationship between loss of energy, mass, and radius of stars in the steady state?
The monograph is divided into two distinct parts. In chapters i-iv, Chandrasekhar presents the "classical" background necessary to his argument: the laws of thermodynamics (from Carathéodory's rigorous axiomatic standpoint), adiabatic and polytropic laws, and the work of Ritter, Emden, Kelvin, and others who developed the applied mathematics of stellar structure. Chapters v-xii discuss modern results: the formal theory of radiation, the equations of radiative equilibrium, the luminosity formula, the theory of stellar envelopes, Gibbs statistical mechanics (the quantum mechanical version), white dwarfs, etc. The closing chapter outlines some general trends in current investigations of the problem.
Appendixes cover physical and astronomical constants; the masses of light atoms; the masses, luminosities, and radii of the stars, derived hydrogen contents, central densities and central temperatures, and tables of white dwarf functions.
"Extremely interesting. It reaches the highest level of scientific merit." — Bulletin, American Mathematical Society.
- Published on: 1958
- Binding: Unknown Binding
- 509 pages
Most helpful customer reviews
20 of 22 people found the following review helpful.
Chandrasekhar on Stellar Structure
By Dimitri Mihalas
This is one of the greatest classics in the astrophysical literature. I bought my first copy of the Dover edition in 1964, when I was a graduate student. I finally
wore it out (the cover fell off), and I was happy to see it still in print by
Dover, so I could buy another.
This book contains Chandra's masterful thoughts about, and analysis of, stellar structure, particularly on the structure of white dwarfs. It was his work at Cambridge in the `30s that showed that the mass of a white dwarf could not exceed a certain limit (universally known as the "Chandrasekhar Limit"), or the relativistically degenerate electrons in its core could not support the weight of the overlying layers, and the star would collapse. In principle the collapse could proceed without limit, and the star could collapse to "a point". This seminal work, for which, ironically, he received the Nobel Prize some 50 or so years later, was ridiculed by Eddington, then regarded as the "most authoritative astrophysicist in Britain", and Chandra chose to immigrate to the United States. (FORTUNATE for us!)
There as a Distinguished Service Professor at the University of Chicago for several decades, he mastered diverse fields, and wrote definitive monographs on Radiative Transfer, Stellar Dynamics, Plasma Physics, and General Relativity. He seemed to take special delight in working on G.R., and produced a virtual faculty-sized group of graduate students all of whom distinguished themeselves in that field.
It is interesting to speculate why R.H. Fowler, also Professor at Cambridge, who with Stoner, who had worked out the theory of relativistic degeneracy (!), did not support Chandra's work against Eddington's illogical attack. It is also interesting to speculate why Chandra did not make the connection between his work and Karl Schwarzschild's previous discovery of the first exact solution of Einstein's equations of general relativity: a singularity in which an amount of matter greater than the "Schwarzschild Limit" collapses to a point, which today we would call a "black hole".
But it must be remembered that an equation of state for matter at nuclear densities and above did not yet exist; and Chandra had such high standards of rigor he would not have time to waste on speculations, nor the temperment to do so.
This book is a jewel. It is required reading for all serious students (at all levels, from first year graduate students to distinguished professors) of astrophysics. In it they will find scientific analysis of the greatest clarity, with the deepest insight, which sets the standard for all subsequent work in the field.
Unfortunately they will not learn about Chandra's incisive clarity on every matter, whether scientific or pracitical, nor about the depth of his humanity and generosity. THAT they should seek to learn from his colleagues who are still alive (Chandra lived into his 80s), and from his many students.
18 of 21 people found the following review helpful.
classic explanations of stars
By W Boudville
This reprint of the 1939 book by Chandrasekhar lets you read through one of the major works on the evolution of a star. The author takes physics equations, labouriously discovered over centuries, in terrestrial environments. He applies them logically to the vastly different circumstances of a star. Yet, step by step, he shows how we can arrive at an understanding of stellar processes that jibes with much that was observable in the 1930s. A tribute to the precision and insight of his thinking, as well as to the power of physics to model phenomena anywhere in the universe.
Actually, in the subsequent decades, the equations derived in the book held up quite well as coherent explanations of stars. While the field has moved on, the explanatory pedagogy given in this book may still often be seen in recent astrophysics texts.
0 of 0 people found the following review helpful.
Five Stars
By RealityQ
Highly recommended
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