Atjaunināt sīkdatņu piekrišanu

E-grāmata: Introduction to the Theory of Stellar Structure and Evolution

4.37/5 (53 ratings by Goodreads)
(Tel-Aviv University)
  • Formāts: PDF+DRM
  • Izdošanas datums: 29-Oct-2009
  • Izdevniecība: Cambridge University Press
  • Valoda: eng
  • ISBN-13: 9781316283165
Citas grāmatas par šo tēmu:
  • Formāts - PDF+DRM
  • Cena: 65,42 €*
  • * ši ir gala cena, t.i., netiek piemērotas nekādas papildus atlaides
  • Ielikt grozā
  • Pievienot vēlmju sarakstam
  • Šī e-grāmata paredzēta tikai personīgai lietošanai. E-grāmatas nav iespējams atgriezt un nauda par iegādātajām e-grāmatām netiek atmaksāta.
Introduction to the Theory of Stellar Structure and EvolutionPalielināt
  • Formāts: PDF+DRM
  • Izdošanas datums: 29-Oct-2009
  • Izdevniecība: Cambridge University Press
  • Valoda: eng
  • ISBN-13: 9781316283165
Citas grāmatas par šo tēmu:

DRM restrictions

  • Kopēšana (kopēt/ievietot):

    nav atļauts

  • Drukāšana:

    nav atļauts

  • Lietošana:

    Digitālo tiesību pārvaldība (Digital Rights Management (DRM))
    Izdevējs ir piegādājis šo grāmatu šifrētā veidā, kas nozīmē, ka jums ir jāinstalē bezmaksas programmatūra, lai to atbloķētu un lasītu. Lai lasītu šo e-grāmatu, jums ir jāizveido Adobe ID. Vairāk informācijas šeit. E-grāmatu var lasīt un lejupielādēt līdz 6 ierīcēm (vienam lietotājam ar vienu un to pašu Adobe ID).

    Nepieciešamā programmatūra
    Lai lasītu šo e-grāmatu mobilajā ierīcē (tālrunī vai planšetdatorā), jums būs jāinstalē šī bezmaksas lietotne: PocketBook Reader (iOS / Android)

    Lai lejupielādētu un lasītu šo e-grāmatu datorā vai Mac datorā, jums ir nepieciešamid Adobe Digital Editions (šī ir bezmaksas lietotne, kas īpaši izstrādāta e-grāmatām. Tā nav tas pats, kas Adobe Reader, kas, iespējams, jau ir jūsu datorā.)

    Jūs nevarat lasīt šo e-grāmatu, izmantojot Amazon Kindle.

"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 stimulating introduction for undergraduates in astronomy, physics and mathematics, this second edition contains two new chapters and new exercises.

Using fundamental physics, the theory of stellar structure and evolution can predict how stars are born, how their complex internal structure changes, what nuclear fuel they burn, and their ultimate fate. This textbook is a stimulating introduction for undergraduates in astronomy, physics and applied mathematics, taking a course on the physics of stars. It uniquely emphasizes the basic physical principles governing stellar structure and evolution. This second edition contains two new chapters on mass loss from stars and interacting binary stars, and new exercises. Clear and methodical, it explains the processes in simple terms, while maintaining mathematical rigor. Starting from general principles, this textbook leads students step-by-step to a global, comprehensive understanding of the subject. Fifty exercises and full solutions allow students to test their understanding. No prior knowledge of astronomy is required, and only a basic background in physics and mathematics is necessary.

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 rigour 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 read 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.' David Hughes, 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 ' a stimulating introduction for students of astronomy, physics and applied mathematics, taking a course on the physics of stars. It uniquely emphasises the basic physical principles governing stellar structure and evolution.' Spaceflight ' second edition of a very popular textbook on stellar structure and evolution The coverage is very comprehensive and well-explained with clear illustrations and interesting historical side notes this textbook is an excellent buy for most students interested in the basic physical properties of stars.' Contemporary Physics

Papildus informācija

A stimulating introduction for undergraduates in astronomy, physics and mathematics, this second edition contains two new chapters and new exercises.
Preface to the second edition xi
Preface to the first edition xiii
1 Observational background and basic assumptions
1
1.1 What is a star?
1
1.2 What can we learn from observations?
2
1.3 Basic assumptions
6
1.4 The H—R diagram: a tool for testing stellar evolution
9
2 The equations of stellar evolution
15
2.1 Local thermodynamic equilibrium
16
2.2 The energy equation
17
2.3 The equation of motion
19
2.4 The virial theorem
21
2.5 The total energy of a star
23
2.6 The equations governing composition changes
25
2.7 The set of evolution equations
28
2.8 The characteristic timescales of stellar evolution
29
3 Elementary physics of gas and radiation in stellar interiors
34
3.1 The equation of state
35
3.2 The ion pressure
37
3.3 The electron pressure
38
3.4 The radiation pressure
42
3.5 The internal energy of gas and radiation
43
3.6 The adiabatic exponent
44
3.7 Radiative transfer
46
4 Nuclear processes that take place in stars
51
4.1 The binding energy of the atomic nucleus
51
4.2 Nuclear reaction rates
53
4.3 Hydrogen burning I: the p — p chain
57
4.4 Hydrogen burning II: the CNO bi-cycle
59
4.5 Helium burning: the triple-a reaction
61
4.6 Carbon and oxygen burning
63
4.7 Silicon burning: nuclear statistical equilibrium
65
4.8 Creation of heavy elements: the s- and r-processes
66
4.9 Pair production
67
4.10 Iron photodisintegration
68
5 Equilibrium stellar configurations — simple models
70
5.1 The stellar structure equations
70
5.2 What is a simple stellar model?
71
5.3 Polytropic models
72
5.4 The Chandrasekhar mass
77
5.5 The Eddington luminosity
78
5.6 The standard model
80
5.7 The point-source model
83
6 The stability of stars
87
6.1 Secular thermal stability
88
6.2 Cases of thermal instability
89
6.3 Dynamical stability
92
6.4 Cases of dynamical instability
94
6.5 Convection
96
6.6 Cases of convective instability
98
6.7 Conclusion
103
7 The evolution of stars — a schematic picture
104
7.1 Characterization of the (log T, log p) plane
105
7.2 The evolutionary path of the central point of a star in the (log T, log p) plane
110
7.3 The evolution of a star, as viewed from its centre
113
7.4 The theory of the main sequence
116
7.5 Outline of the structure of stars in late evolutionary stages
122
7.6 Shortcomings of the simple stellar evolution picture
126
8 Mass loss from stars
130
8.1 Observational evidence of mass loss
130
8.2 The mass loss equations
131
8.3 Solutions to the wind equations – the isothermal case
136
8.4 Mass loss estimates
139
8.5 Empirical solutions
142
9 The evolution of stars – a detailed picture
144
9.1 The Hayashi zone and the pre-main-sequence phase
145
9.2 The main-sequence phase
151
9.3 Solar neutrinos
155
9.4 The red giant phase
160
9.5 Helium burning in the core
165
9.6 Thermal pulses and the asymptotic giant branch
168
9.7 The superwind and the planetary nebula phase
173
9.8 White dwarfs: the final state of nonmassive stars
177
9.9 The evolution of massive stars
182
9.10 The H–R diagram – Epilogue
186
10 Exotic stars: supernovae, pulsars and black holes 189
10.1 What is a supernova?
189
10.2 Iron-disintegration supernovae: Type II – the fate of massive stars
193
10.3 Nucleosynthesis during Type II supernova explosions
197
10.4 Supernova progenies: neutron stars – pulsars
200
10.5 Carbon-detonation supernovae: Type Ia
204
10.6 Pair-production supernovae and black holes – the fate of very massive stars
205
11 Interacting binary stars 208
11.1 What is a binary star?
208
11.2 The general effects of stellar binarity
211
11.3 The mechanics of mass transfer between stars
216
11.4 Conservative mass transfer
219
11.5 Accretion discs
220
11.6 Cataclysmic phenomena: Nova outbursts
223
12 The stellar life cycle 231
12.1 The interstellar medium
231
12.2 Star formation
232
12.3 Stars, brown dwarfs and planets
236
12.4 The initial mass function
239
12.5 The global stellar evolution cycle
243
Appendix A The equation of radiative transfer 251
Appendix B The equation of state for degenerate electrons 259
Appendix C Solutions to all the exercises 270
Appendix D Physical and astronomical constants and conversion factors 300
Bibliography 303
Index 308
Dina Prialnik is a Professor of Planetary Physics at Tel Aviv University. Her research interests lie in stellar evolution; the structure and evolution of cataclysmic variables, comet nuclei and other small Solar System bodies; and the evolution of planets.
Biežāk uzdotie jautājumi par e-grāmatām Biežāk uzdotie jautājumi par e-grāmatām
Permanent link: https://www.kriso.lv/db/97813162831652e.html
Keywords: