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E-raamat: Stellar Evolution Physics: Volume 1, Physical Processes in Stellar Interiors

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(University of Illinois, Urbana-Champaign)
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Stellar Evolution Physics: Volume 1, Physical Processes in Stellar InteriorsSuurem pilt
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This text describes the microscopic physics operating in stars and demonstrates how stars respond from formation, through hydrogen-burning phases, up to the onset of helium burning. Intended for beginning graduate students and senior undergraduates with a solid background in physics, it illustrates the intricate interplay between the microscopic physical processes and the stars' macroscopic responses. The volume starts with the gravitationally contracting phase which carries the star from formation to the core hydrogen-burning main sequence, through the main sequence phase, through shell hydrogen-burning phases as a red giant, up to the onset of core helium burning. Particular emphasis is placed on describing the gravothermal responses of stars to nuclear transformations in the interior and energy loss from the surface, responses which express the very essence of stellar evolution. The volume is replete with many illustrations and detailed numerical solutions to prepare the reader to program and calculate evolutionary models.

Arvustused

'This is a book by one of the most prolific researchers in the area of stellar evolution, and he has plenty to teach practitioners in the field [ the] style is always clear and straightforward This is not a book for the faint-hearted, but it is certainly full of fascinating detail which will repay study by the active researcher Iben has produced a classic monograph, which compares well with classics of the past, and I am pleased to have a copy.' The Observatory

Muu info

Describes how stars respond to microscopic physics, from formation, through hydrogen-burning phases, up to the onset of helium burning.
Preface xiii
Bibliography and references xvi
Part I Introduction and overview
1(54)
1 Qualitative description of single and binary star evolution
3(27)
1.1 On the evolutionary status of real single stars
5(9)
1.2 Close binary stars and evolutionary scenarios
14(16)
Bibliography and references
28(2)
2 Quantitative foundations of stellar evolution theory
30(25)
2.1 Observed properties of the Sun
30(8)
2.2 Nearby stars in the Hertzsprung--Russell diagram
38(3)
2.3 Mass--luminosity relationships
41(4)
2.4 Evolutionary paths of theoretical models in the HR diagram
45(6)
2.5 The evolutionary status of familiar stars
51(4)
Bibliography and references
54(1)
Part II Basic physical processes in stellar interiors
55(472)
3 Properties of and physical processes in main sequence stars -- order of magnitude estimates
57(31)
3.1 Particle numbers and separations, pressures and temperatures
58(3)
3.2 Departures from a classical perfect gas: electrostatic interactions, electron degeneracy, and radiation pressure
61(4)
3.2.1 Electrostatic forces
61(1)
3.2.2 The exclusion principle and electron degeneracy
62(2)
3.2.3 Radiation pressure
64(1)
3.3 Virial theorems relating kinetic, gravitational binding, and net binding energies
65(3)
3.4 Energy transport: radiation, convection, and conduction
68(12)
3.4.1 Radiative flow and mass--luminosity relationships
69(2)
3.4.2 Opacity sources
71(2)
3.4.3 Convection
73(5)
3.4.4 Heat conduction by electrons
78(2)
3.4.5 Summary
80(1)
3.5 Nuclear energy-generation rates and evolutionary time scales
80(6)
3.6 The static electrical field
86(2)
Bibliography and references
87(1)
4 Statistical mechanics, thermodynamics, and equations of state
88(103)
4.1 Quantum-mechanical wave functions and the unit cell in phase space
89(2)
4.2 The connection between thermodynamics and Fermi--Dirac statistics for particles which obey the Pauli exclusion principle
91(6)
4.3 Calculation of pressure and energy density
97(2)
4.4 Equation of state for non-degenerate, non-relativistic ions
99(2)
4.5 Equation of state for weakly degenerate, non-relativistic electrons
101(4)
4.6 Equation of state for strongly degenerate, non-relativistic electrons
105(5)
4.7 Equation of state for non-relativistic electrons of intermediate degeneracy
110(6)
4.8 Equation of state for relativistically degenerate electrons at zero temperature
116(5)
4.9 Equation of state for relativistically degenerate electrons at finite temperatures
121(7)
4.10 High temperatures and electron--positron pairs
128(21)
4.11 Indistinguishable particles, Bose--Einstein statistics, and the electromagnetic radiation field
149(5)
4.12 Maxwell--Boltzmann statistics and entropy
154(4)
4.13 Ionization equilibrium and the Saha equation for pure hydrogen
158(7)
4.14 Thermodynamic properties of partially ionized hydrogen
165(5)
4.15 The generalized Saha equations, with application to pure helium
170(4)
4.16 Thermodynamic properties of hydrogen- and helium-rich matter in stellar envelopes
174(5)
4.17 The effect of Coulomb interactions on the equation of state for a gas
179(12)
4.17.1 Modifications when electrons are modestly degenerate
184(3)
4.17.2 When electrons are significantly degenerate
187(2)
Bibliography and references
189(2)
5 Polytropes and single zone models
191(67)
5.1 The basic structure equation when pressure is proportional to a fixed power (1 + 1/N) of the density
193(4)
5.2 Several properties of solutions as functions of N
197(13)
5.3 Additional properties of solutions when an equation of state and a law of nuclear energy generation are assumed
210(5)
5.4 Luminosity as a function of position in core nuclear burning models
215(7)
5.5 Polytropic characteristics of zero age main sequence models
222(2)
5.6 Models in adiabatic equilibrium: existence of a maximum temperature and decrease of entropy with time
224(7)
5.7 White dwarf properties revealed by polytropes: radius--mass relationships and the maximum mass
231(6)
5.7.1 Consequences of the N = 3/2 polytropic approximation
232(3)
5.7.2 The Chandrasekhar mass limit from the N = 3 polytrope
235(2)
5.8 Insights from one zone models: white dwarf radius versus mass, heating and cooling in a low mass star as functions of radius, and compression and ion cooling as luminosity sources in white dwarfs
237(11)
5.8.1 The temperature maximum and the nature of energy sources in cooling white dwarfs and completely convective low mass stars
242(6)
5.9 One zone models of neutron stars, neutron star composition, and neutron star masses
248(10)
Bibliography and references
256(2)
6 Hydrogen-burning reactions and energy-generation rates
258(40)
6.1 The nature and energetics of the pp reaction
260(1)
6.2 Ingredients of the pp-reaction probability
261(1)
6.3 An estimate of the weak interaction coupling constant
262(2)
6.4 The nuclear matrix element
264(4)
6.5 A numerical estimate of the cross section
268(1)
6.6 The pp-reaction rate and proton lifetime
269(2)
6.7 Other hydrogen-burning reactions -- laboratory cross sections and extrapolation to stellar conditions
271(4)
6.8 The pp-chain reactions
275(5)
6.9 Equilibrium abundances and energy-generation rates for pp-chain reactions
280(4)
6.10 The CN-cycle reactions
284(3)
6.11 The effect of electrostatic screening on nuclear reaction rates
287(4)
6.12 Polytropic models for zero age main sequence stars
291(7)
Bibliography and references
297(1)
7 Photon--matter interaction probabilities, absorption cross sections, and opacity
298(137)
7.1 Photons and the electron--photon interaction Hamiltonian
300(3)
7.2 First order perturbation theory and the golden rule for a radiative transition between two matter eigenstates
303(4)
7.3 The relationship between emission and absorption probabilities
307(5)
7.4 The cross section for bound--free (photoelectric) absorption from the K shell
312(7)
7.4.1 On the determination of the associated opacity coefficient
319(1)
7.5 The matrix element for free-free (inverse bremsstrahlung) absorption
319(6)
7.6 The cross section for free--free absorption
325(6)
7.7 The Kramers semiclassical approximation and Gaunt factors for free--free absorption
331(6)
7.8 Spontaneous emission between bound atomic states
337(4)
7.9 Detailed balance, stimulated emission, bound--bound cross sections, and line broadening
341(6)
7.10 The Rosseland mean opacity
347(3)
7.11 Sample calculations of the Rosseland mean opacity
350(30)
7.11.1 Hydrogen and helium completely ionized, oxygen with zero to two bound electrons
351(3)
7.11.2 Anatomy of an opacity when density = 1 g cm-3 and temperature varies from 107 to 106 K
354(7)
7.11.3 Arbitrary states of ionization for hydrogen, helium, and oxygen
361(2)
7.11.4 Number abundances and opacities as functions of temperature when density = 0.01 g cm-3
363(8)
7.11.5 Number abundances and opacities as functions of temperature when density = 10-4 g cm-3
371(5)
7.11.6 Number abundances and opacities as functions of temperature when density = 10-6 g cm-3
376(1)
7.11.7 The effect on the Rosseland mean opacity of using Coulomb-distorted plane waves for electrons to obtain the free--free absorption coefficient
377(2)
7.11.8 Concluding comments
379(1)
7.12 Analytical approximations to results of opacity calculations for intermediate to high temperatures
380(8)
7.12.1 Keller--Meyerott opacities
381(1)
7.12.2 Metal-free opacities at high temperatures
382(2)
7.12.3 Cox--Stewart opacities at intermediate to high temperatures for mixtures of hydrogen and helium when Z < 0.02
384(1)
7.12.4 Cox--Stewart opacities at high temperatures for mixtures of helium, carbon, and oxygen
385(3)
7.13 Convective cores in stars burning nuclear fuel at the center
388(11)
7.13.1 The criterion for convection at the center and evidence for the composite nature of models relying on CN-cycle energy generation
389(3)
7.13.2 Estimates of the size of a convection core in CN-cycle-burning main sequence stars
392(3)
7.13.3 Convective regions in realistic models of zero age main sequence models
395(4)
7.14 Algorithms for interpolation in opacity tables
399(16)
7.14.1 Linear interpolation
399(2)
7.14.2 Quadratic interpolation
401(3)
7.14.3 Cubic spline interpolation
404(6)
7.14.4 Bicubic spline interpolation
410(5)
7.15 Interpolation in opacity tables: a concrete example
415(4)
7.16 Absorption by the negative hydrogen ion
419(16)
Bibliography and references
433(2)
8 Equations of stellar evolution and methods of solution
435(92)
8.1 Consequences of the conservation of mass, momentum, and energy
437(9)
8.2 Examples of the creation--destruction potential for ions and electrons
446(7)
8.3 The quasistatic equations of stellar structure in spherical symmetry
453(4)
8.4 The photospheric boundary condition
457(2)
8.5 The classical fitting technique for model construction
459(3)
8.5.1 Development close to the model center and near the surface
459(1)
8.5.2 Matching results of inward and outward integrations
460(2)
8.6 On the construction of integration algorithms
462(15)
8.6.1 Application to stellar structure
476(1)
8.7 The relaxation technique for model construction
477(16)
8.8 Composition changes in radiative regions due to nuclear transformations
493(7)
8.9 Solution of linear equations by Gaussian elimination and LU decomposition
500(6)
8.10 Composition changes in convective regions
506(10)
8.10.1 Time scales of relevance
507(1)
8.10.2 Convective diffusion in the mixing length approximation
508(3)
8.10.3 Solution of the convective diffusion equation: conversion to a difference equation and construction of recurrence relationships
511(2)
8.10.4 The outer boundary condition and the quantities ak and bk
513(2)
8.10.5 The inner boundary condition and determination of new composition variables
515(1)
8.10.6 Composition in the static envelope
516(1)
8.11 Remarks on mixing in radiative zones due to particle diffusion: gravitational settling, abundance-gradient induced diffusion and rotation-induced diffusion
516(3)
8.12 Zoning considerations and choice of time step
519(2)
8.13 On the evolution of the computing environment
521(6)
Bibliography and references
525(2)
Part III Pre-main sequence, main sequence, and shell hydrogen-burning evolution of single stars
527(319)
9 Star formation, pre-main sequence evolution, and the zero age main sequence
529(108)
9.1 Some concepts relevant to star formation
531(8)
9.1.1 The Jeans criterion
531(3)
9.1.2 The roles of magnetic fields and cosmic rays
534(1)
9.1.3 Other studies of collapse and formation of a quasistatic core
535(3)
9.1.4 Further description of the accretion phase
538(1)
9.2 Pre-main sequence quasistatic evolution of a solar mass population I model with deuterium burning
539(34)
9.2.1 Input physics and initial abundances for evolutionary calculations
540(3)
9.2.2 Structure and gravothermal characteristics of a Hayashi-band model
543(5)
9.2.3 The deuterium-burning phase
548(8)
9.2.4 Evolution in the HR diagram and characteristics of models along the approximately vertical portion of the track
556(7)
9.2.5 Development of a radiative core and the transition from vertically downward to upward and leftward in the HR diagram
563(3)
9.2.6 Characteristics of a model in transition from the convective phase to the predominantly radiative phase
566(7)
9.3 Approach of a solar mass model to the main sequence: the onset and ascendancy of hydrogen burning by pp-chain reactions and properties of a zero-age main sequence model
573(24)
9.3.1 Hydrogen burning begins
573(6)
9.3.2 A model in which nuclear burning and gravitational work contribute comparably to the surface luminosity
579(8)
9.3.3 A zero age main sequence model
587(10)
9.4 Evolution of a 5 M population I model to the main sequence: gravitational contraction, C → N burning, CN-cycle burning, and properties of a zero age main sequence model
597(25)
9.5 Evolution of a 25 M gravitationally contracting population I model through deuterium burning and two C rarr; N burning phases, and properties of a CN-cycle burning zero age main sequence model
622(15)
Bibliography and references
635(2)
10 Solar structure and neutrino physics
637(77)
10.1 Construction and properties of a Z = 0.01 solar-like model with the Sun's luminosity, radius, and estimated age
639(19)
10.2 Construction and properties of a Z = 0.02 solar-like model with the Sun's luminosity, radius, and estimated age, and comparisons with the Z = 0.01 solar-like model
658(10)
10.3 Contributions to photon and neutrino luminosities and to neutrino fluxes at the Earth
668(5)
10.4 The solar neutrino problem
673(9)
10.5 Neutrino oscillations in vacuum
682(7)
10.6 The MSW effect
689(10)
10.7 Numerical solutions for neutrinos produced at the center of a simple solar model
699(4)
10.8 Solutions for neutrinos produced in realistic solar models
703(7)
10.9 Summary and conclusions
710(1)
10.10 Postscript
711(3)
Bibliography and references
712(2)
11 Evolution through hydrogen-burning phases of models of mass 1, 5, and 25 M
714(132)
11.1 Evolution of a 1 M model during core and shell hydrogen burning on the main sequence, formation of an electron-degenerate core, and core growth during shell hydrogen burning on the red giant branch
716(52)
11.2 Evolution of a 5 M model during core hydrogen burning, development of a thick hydrogen-burning shell, and shell hydrogen-burning evolution up to the onset of core helium burning as a red giant
768(52)
11.3 Evolution of a 25 M model without mass loss during core hydrogen burning on the main sequence and during shell hydrogen burning near the main sequence up to the onset of core helium burning as a blue giant
820(16)
11.4 Global properties of main sequence models as functions of model mass and estimates of surface mass loss during pure hydrogen-burning phases
836(10)
11.4.1 Global main sequence properties
836(4)
11.4.2 Mass loss during hydrogen-burning phases
840(5)
Bibliography and references
845(1)
Index 846
Icko Iben, Jr is Emeritus Distinguished Professor of Astronomy and Physics at the University of Illinois, Urbana-Champaign, where he also gained his MS and PhD degrees in Physics and where a Distinguished Lectureship in his name was established in 1998. He initiated his teaching career at Williams College (19581961), engaged in astrophysics research as a Senior Research Fellow at Cal Tech (19611964), and continued his teaching career at the Massachusetts Institute of Technology (19641972) and Illinois (19721999). He has held visiting Professorships at over a dozen institutions, including Harvard University, the University of California, Santa Cruz, the University of Bologna, Italy and Niigata University, Japan. He was elected to the US National Academy of Sciences in 1985 and his awards include the Russell Lectureship of the American Astronomical Society (1989), the George Darwin Lectureship (1984) and the Eddington Medal (1990) of the Royal Astronomical Society, and the Eminent Scientist Award of the Japan Society for the Promotion of Science (20032004).
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