Introduction to the Theory of Stellar Structure and Evolution

ISBN-10: 0521866049
ISBN-13: 9780521866040
Edition: 2nd 2009 (Revised)
Authors: Dina Prialnik
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Book details

List price: $105.00
Edition: 2nd
Copyright year: 2009
Publisher: Cambridge University Press
Publication date: 10/29/2009
Binding: Hardcover
Pages: 328
Size: 7.00" wide x 10.00" long x 0.75" tall
Weight: 1.188
Language: English

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.

Preface to the second edition page
Preface to the first edition
Observational background and basic assumptions
What is a star?
What can we learn from observations?
Basic assumptions
The H-R diagram: a tool for testing stellar evolution
The equations of stellar evolution
Local thermodynamic equilibrium
The energy equation
The equation of motion
The virial theorem
The total energy of a star
The equations governing composition changes
The set of evolution equations
The characteristic timescales of stellar evolution
Elementary physics of gas and radiation in stellar interiors
The equation of state
The ion pressure
The electron pressure
The radiation pressure
The internal energy of gas and radiation
The adiabatic exponent
Radiative transfer
Nuclear processes that take place in stars
The binding energy of the atomic nucleus
Nuclear reaction rates
Hydrogen burning I: the p - p chain
Hydrogen burning II: the CNO bi-cycle
Helium burning: the triple-a reaction
Carbon and oxygen burning
Silicon burning: nuclear statistical equilibrium
Creation of heavy elements: the s- and r-processes
Pair production
Iron photodisintegration
Equilibrium stellar configurations - simple models
The stellar structure equations
What is a simple stellar model?
Polytropic models
The Chandrasekhar mass
The Eddington luminosity
The standard model
The point-source model
The stability of stars
Secular thermal stability
Cases of thermal instability
Dynamical stability
Cases of dynamical instability
Convection
Cases of convective instability
Conclusion
The evolution of stars - a schematic picture
Characterization of the (log T, log p) plane
The evolutionary path of the central point of a star in the (log T, log p) plane
The evolution of a star, as viewed from its centre
The theory of the main sequence
Outline of the structure of stars in late evolutionary stages
Shortcomings of the simple stellar evolution picture
Mass loss from stars
Observational evidence of mass loss
The mass loss equations
Solutions to the wind equations - the isothermal case
Mass loss estimates
Empirical solutions
The evolution of stars - a detailed picture
The Hayashi zone and die pre-main-sequence phase
The main-sequence phase
Solar neutrinos
The red giant phase
Helium burning in the core
Thermal pulses and the asymptotic giant branch
The superwind and the planetary nebula phase
White dwarfs: the final state of nonmassive stars
The evolution of massive stars
The H-R diagram - Epilogue
Exotic stars: supernovae, pulsars and black holes
What is a supernova?
Iron-disintegration supernovae: Type II - the fate of massive stars
Nucleosynthesis during Type II supernova explosions
Supernova progenies: neutron stars - pulsars
Carbon-detonation supernovae: Type Ia
Pair-production supernovae and black holes - the fate of very massive stars
Interacting binary stars
What is a binary star?
The general effects of stellar binarity
The mechanics of mass transfer between stars
Conservative mass transfer
Accretion discs
Cataclysmic phenomena: Nova outbursts
The stellar life cycle
The interstellar medium
Star formation
Stars, brown dwarfs and planets
The initial mass function
The global stellar evolution cycle
The equation of radiative transfer
The equation of state for degenerate electrons
Solutions to all the exercises
Physical and astronomical constants and conversion factors

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