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Introduction to the Theory of Stellar Structure and Evolution [Mīkstie vāki]

4.37/5 (58 ratings by Goodreads)
(Tel-Aviv University)
  • Formāts: Paperback / softback, 276 pages, height x width x depth: 254x178x19 mm, weight: 500 g, Worked examples or Exercises; 12 Tables, unspecified; 10 Halftones, unspecified; 60 Line drawings, unspecified
  • Izdošanas datums: 24-Jul-2000
  • Izdevniecība: Cambridge University Press
  • ISBN-10: 052165937X
  • ISBN-13: 9780521659376
Citas grāmatas par šo tēmu:
  • Mīkstie vāki
  • Cena: 52,11 €
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  • Formāts: Paperback / softback, 276 pages, height x width x depth: 254x178x19 mm, weight: 500 g, Worked examples or Exercises; 12 Tables, unspecified; 10 Halftones, unspecified; 60 Line drawings, unspecified
  • Izdošanas datums: 24-Jul-2000
  • Izdevniecība: Cambridge University Press
  • ISBN-10: 052165937X
  • ISBN-13: 9780521659376
Citas grāmatas par šo tēmu:
"Stellar evolution calculations have made great progress in recent years, following the rapid development of computational means: increasingly faster CPUs and greater memory volumes. Nevertheless, I have made use of new results only when they provide better illustration for points raised in text. For themost part, old results are still valid and this long-term validity is worth emphasizing; the theory of stellar structure and evolution, with all its complexity, is a well-established physical theory. The text was"--Provided by publisher.

A lucid introductory textbook for undergraduate students in physics, astronomy, planetary science and applied mathematics taking a course on the physics of stars.

Using fundamental physics, the theory of stellar structure and evolution is able to predict how stars are born, how their complex internal structure changes, what nuclear fuel they burn, and their ultimate fate. This undergraduate textbook provides a clear, methodical introduction to the theory of stellar structure and evolution. Starting from general principles and axioms, step-by-step coverage leads students to a global, comprehensive understanding of the subject. Throughout, the book uniquely places emphasis on the basic physical principles governing stellar structure and evolution. All processes are explained in clear and simple terms with all the necessary mathematics included. Exercises and their full solutions allow students to test their understanding. This book requires only a basic background in physics and mathematics and assumes no prior knowledge of astronomy. It provides a stimulating introduction for undergraduates in astronomy, physics, planetary science and applied mathematics taking a course on the physics of stars.

Recenzijas

'The unique feature of this book is the emphasis it places, throughout, on the basic physical principles governing stellar evolution. The processes are always explained in the simplest terms, while maintaining full mathematical rigor This textbook provides a stimulating introduction for undergraduates in astronomy, physics, planetary science, and applied mathematics who are taking a course on the physics of stars. Because this book requires only basic undergraduate physics and mathematics and no prior knowledge of astronomy it may be written by advanced amateurs as well.' Orion 'Here we have a first-class textbook that spells out in a clear and methodical way the principles that underlie the life cycles of stars and the physics of their interiors. The host of student exercises in this book, plus the useful worked answers, ensure that any dedicated physics or mathematics undergraduate can, with some effort, understand what is going on.' New Scientist 'To my mind, this is the first book to be both a candidate for the title of classic and at the same time suitable for undergraduates The approach is very different from that of most textbooks on stars Throughout the book, the emphasis is on understanding physical principles, and there are well-designed exercises scattered through the text, relating to material that has just been covered; full solutions are clearly set out in an appendix This is a book that I can strongly recommend as a suitable textbook to anyone teaching a course in stellar structure, at advanced undergraduate or beginning graduate level Any undergraduate who masters this book will not only be well prepared to undertake graduate work in the area but will also understand his/her other physics courses better. An excellent book, which certainly deserves to become a classic.' Robert Connon Smith, The Observatory

Papildus informācija

A lucid introductory textbook for undergraduate students in physics, astronomy, planetary science and applied mathematics taking a course on the physics of stars.
Preface xi
Observational background and basic assumptions
1(14)
What is a star?
1(1)
What can we learn from observations?
2(4)
Basic assumptions
6(3)
The H-R diagram: a tool for testing stellar evolution
9(6)
The equations of stellar evolution
15(20)
Local thermodynamic equilibrium
16(1)
The energy equation
17(2)
The equation of motion
19(2)
The virial theorem
21(3)
The total energy of a star
24(2)
The equations governing composition changes
26(3)
The set of evolution equations
29(1)
The characteristic timescales of stellar evolution
30(5)
Elementary physics of gas and radiation in stellar interiors
35(18)
The equation of state
36(2)
The ion pressure
38(1)
The electron pressure
39(4)
The radiation pressure
43(1)
The internal energy of gas and radiation
44(1)
The adiabatic exponent
45(3)
Radiative transfer
48(5)
Nuclear processes that take place in stars
53(19)
The binding energy of the atomic nucleus
53(3)
Nuclear reaction rates
56(3)
Hydrogen burning I: the p-p chain
59(3)
Hydrogen burning II: the CNO bi-cycle
62(1)
Helium burning: the triple-a reaction
63(2)
Carbon and oxygen burning
65(2)
Silicon burning: nuclear statistical equilibrium
67(1)
Creation of heavy elements: the s-and r-processes
68(2)
Pair production
70(1)
Iron photodisintegration
70(2)
Equilibrium stellar configurations - simple models
72(18)
The stellar structure equations
72(1)
What is a simple stellar model?
73(1)
Polytropic models
74(5)
The Chandrasekhar mass
79(2)
The Eddington luminosity
81(1)
The standard model
82(4)
The point-source model
86(4)
The stability of stars
90(16)
Secular thermal stability
90(2)
Cases of thermal instability
92(3)
Dynamical stability
95(2)
Cases of dynamical instability
97(1)
Convection
98(3)
Cases of convective instability
101(3)
Conclusion
104(2)
The evolution of stars - a schematic picture
106(25)
Characterization of the (log T, log p) plane
107(4)
The evolutionary path of the central point of a star in the (log T, log p) plane
111(4)
The evolution of a star, as viewed from its centre
115(3)
The theory of the main sequence
118(6)
Outline of the structure of stars in late evolutionary stages
124(4)
Shortcomings of the simple stellar evolution picture
128(3)
The evolution of stars - a detailed picture
131(45)
The Hayashi zone and the pre-main-sequence phase
132(6)
The main-sequence phase
138(5)
Solar neutrinos
143(3)
The red giant phase
146(5)
Helium burning in the core
151(4)
Thermal pulses and the asymptotic giant branch
155(5)
The superwind and the planetary nebula phase
160(4)
White dwarfs - the final state of nonmassive stars
164(6)
The evolution of massive stars
170(3)
The H-R diagram: Epilogue
173(3)
Exotic stars: supernovae, pulsars, and black holes
176(19)
What is a supernova?
176(4)
Supernova explosions - the fate of massive stars
180(4)
Nucleosynthesis during supernova explosions
184(3)
Supernova progenies: neutron stars - pulsars
187(4)
Very massive stars and black holes
191(1)
The luminosity of accretion and hard radiation sources
192(3)
The stellar life cycle
195(56)
The interstellar medium
195(1)
Star formation
196(3)
Stars, brown dwarfs, and planets
199(4)
The initial mass function
203(5)
The global stellar evolution cycle
208(7)
Appendices
1 The equation of radiative transfer
215(8)
2 Solutions to all the exercises
223(26)
3 Physical and astronomical constants
249(2)
Bibliography 251(4)
Index 255