恒星结构与演化(第2版)(英文影印版)

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Part I The Basic Equations 1 Coordinates, Mass Distribution, and Gravitational Field in Spherical Stars 3 11 Eulerian Description 3 12 Lagrangian Description 4 13 The Gravitational Field 6 2 Conservation of Momentum9 21 Hydrostatic Equilibrium9 22 The Role of Density and Simple Solutions 10 23 Simple Estimates of Central Values Pc； Tc 12 24 The Equation of Motion for Spherical Symmetry 13 25 The Non-spherical Case 15 26 Hydrostatic Equilibrium in General Relativity 15 27 The Piston Model 17 3 The Virial Theorem 19 31 Stars in Hydrostatic Equilibrium 19 32 The Virial Theorem of the Piston Model21 33 The Kelvin-Helmholtz Timescale 22 34 The Virial Theorem for Non-vanishing Surface Pressure 23 4 Conservation of Energy 25 41 Thermodynamic Relations 25 42 The Perfect Gas and the Mean MolecularWeight 28 43 Thermodynamic Quantities for the Perfect, Monatomic Gas 30 44 Energy Conservation in Stars31 45 Global and Local Energy Conservation33 46 Timescales35 5 Transport of Energy by Radiation and Conduction 37 51 Radiative Transport of Energy 37 511 Basic Estimates 37 512 Diffusion of Radiative Energy38 513 The Rosseland Mean for __ 40 52 Conductive Transport of Energy 42 53 The Thermal Adjustment Time of a Star43 54 Thermal Properties of the Piston Model 45 6 Stability Against Local, Non-spherical Perturbations47 61 Dynamical Instability 47 62 Oscillation of a Displaced Element 52 63 Vibrational Stability 54 64 The Thermal Adjustment Time 55 65 Secular Instability 56 66 The Stability of the Piston Model58 7 Transport of Energy by Convection61 71 The Basic Picture 62 72 Dimensionless Equations 65 73 Limiting Cases, Solutions, Discussion 66 74 Extensions of the Mixing-Length Theory 70 8 The Chemical Composition 73 81 Relative Mass Abundances 73 82 Variation of Composition with Time 74 821 Radiative Regions 74 822 Diffusion 76 823 Convective Regions 80 9 Mass Loss 83 Part II The Overall Problem 10 The Differential Equations of Stellar Evolution 89 101 The Full Set of Equations89 102 Timescales and Simplifications 91 11 Boundary Conditions93 111 Central Conditions 93 112 Surface Conditions95 113 Influence of the Surface Conditions and Properties of Envelope Solutions 98 1131 Radiative Envelopes 98 1132 Convective Envelopes 101 1133 Summary102 1134 The T _r Stratification 102 12 Numerical Procedure 105 121 The ShootingMethod 105 122 The Henyey Method 106 123 Treatment of the First- and Second-Order Time Derivatives 113 124 Treatment of the Diffusion Equation 115 125 Treatment of Mass Loss 117 126 Existence and Uniqueness 118 Part III Properties of Stellar Matter 13 The Perfect Gas with Radiation123 131 Radiation Pressure123 132 Thermodynamic Quantities 124 14 Ionization127 141 The Boltzmann and Saha Formulae 127 142 Ionization of Hydrogen 130 143 Thermodynamical Quantities for a Pure Hydrogen Gas132 144 Hydrogen-HeliumMixtures 133 145 The General Case 135 146 Limitation of the Saha Formula 137 15 The Degenerate Electron Gas 139 151 Consequences of the Pauli Principle 139 152 The Completely Degenerate Electron Gas 140 153 Limiting Cases144 154 Partial Degeneracy of the Electron Gas 145 16 The Equation of State of Stellar Matter 151 161 The Ion Gas 151 162 The Equation of State 152 163 Thermodynamic Quantities 154 164 Crystallization 157 165 Neutronization158 166 Real Gas Effects 159 17 Opacity 163 171 Electron Scattering 163 172 Absorption Due to Free-Free Transitions 164 173 Bound-Free Transitions 165 174 Bound-Bound Transitions166 175 The Negative Hydrogen Ion 168 176 Conduction169 177 Molecular Opacities 170 178 Opacity Tables172 18 Nuclear Energy Production 175 181 Basic Considerations175 182 Nuclear Cross Sections 179 183 Thermonuclear Reaction Rates 182 184 Electron Shielding188 185 The Major Nuclear Burning Stages 192 1851 Hydrogen Burning 193 1852 Helium Burning 197 1853 Carbon Burning and Beyond 199 186 Neutron-Capture Nucleosynthesis 201 187 Neutrinos 205 Part IV Simple Stellar Models 19 Polytropic Gaseous Spheres 213 191 Polytropic Relations 213 192 Polytropic Stellar Models215 193 Properties of the Solutions 216 194 Application to Stars 218 195 Radiation Pressure and the Polytrope n D 3219 196 Polytropic Stellar Models with Fixed K 220 197 Chandrasekhar's Limiting Mass 221 198 Isothermal Spheres of an Ideal Gas 222 199 Gravitational and Total Energy for Polytropes 224 1910 Supermassive Stars 226 1911 A Collapsing Polytrope 227 20 Homology Relations 233 201 Definitions and Basic Relations 233 202 Applications to Simple Material Functions 237 2021 The Case ? D 0 237 2022 The Case ? D ? D ' D 1； a D b D 0 237 2023 The Role of the Equation of State 239 203 Homologous Contraction 241 21 Simple Models in the U-V Plane 243 211 The U-V Plane 243 212 Radiative Envelope Solutions246 213 Fitting of a Convective Core 248 214 Fitting of an Isothermal Core 250 22 The Zero-AgeMain Sequence 251 221 Surface Values251 222 Interior Solutions 254 223 Convective Regions 258 224 Extreme Values of M 260 225 The Eddington Luminosity 261 23 Other Main Sequences 263 231 The Helium Main Sequence 263 232 The Carbon Main Sequence 266 233 Generalized Main Sequences 267 24 The Hayashi Line 271 241 Luminosity of Fully ConvectiveModels272 242 A Simple Description of the Hayashi Line 273 243 The Neighbourhood of the Hayashi Line and the Forbidden Region276 244 Numerical Results279 245 Limitations for Fully ConvectiveModels281 25 Stability Considerations 283 251 General Remarks 283 252 Stability of the Piston Model 285 2521 Dynamical Stability 285 2522 Inclusion of Non-adiabatic Effects 286 253 Stellar Stability288 2531 Perturbation Equations 289 2532 Dynamical Stability 290 2533 Non-adiabatic Effects 292 2534 The Gravothermal Specific Heat 293 2535 Secular Stability Behaviour of Nuclear Burning 294 Part V Early Stellar Evolution 26 The Onset of Star Formation 299 261 The Jeans Criterion 299 2611 An Infinite Homogeneous Medium299 2612 A Plane-Parallel Layer in Hydrostatic Equilibrium 302 262 Instability in the Spherical Case 303 263 Fragmentation 307 27 The Formation of Protostars311 271 Free-Fall Collapse of a Homogeneous Sphere 311 272 Collapse onto a Condensed Object 313 273 A Collapse Calculation 314 274 The Optically Thin Phase and the Formation of a Hydrostatic Core 315 275 Core Collapse 317 276 Evolution in the Hertzsprung-Russell Diagram 320 28 Pre-Main-Sequence Contraction 323 281 Homologous Contraction of a Gaseous Sphere323 282 Approach to the Zero-Age Main Sequence326 29 From the Initial to the Present Sun 329 291 Known Solar Data329 292 Choosing the Initial Model 331 293 A Standard Solar Model 333 294 Results of Helioseismology 336 295 Solar Neutrinos 338 30 Evolution on the Main Sequence 343 301 Change in the Hydrogen Content343 302 Evolution in the Hertzsprung-Russell Diagram 346 303 Timescales for Central Hydrogen Burning 347 304 Complications Connected with Convection 348 3041 Convective Overshooting 349 3042 Semiconvection354 305 The Sch¨onberg-Chandrasekhar Limit 356 3051 A Simple Approach: The Virial Theorem and Homology 358 3052 Integrations for Core and Envelope360 3053 Complete Solutions for Stars with Isothermal Cores 361 Part VI Post-Main-Sequence Evolution 31 Evolution Through Helium Burning: Intermediate-Mass Stars367 311 Crossing the Hertzsprung Gap 367 312 Central Helium Burning 371 313 The Cepheid Phase 375 314 To Loop or Not to Loop : : : 378 315 After Central Helium Burning 384 32 Evolution Through Helium Burning: Massive Stars 385 321 Semiconvection 385 322 Overshooting387 323 Mass Loss 389 33 Evolution Through Helium Burning: Low-Mass Stars 391 331 Post-Main-Sequence Evolution 391 332 Shell-Source Homology 392 333 Evolution Along the Red Giant Branch 397 334 The Helium Flash 401 335 Numerical Results for the Helium Flash 402 336 Evolution After the Helium Flash407 337 Evolution from the Zero-Age Horizontal Branch 410 Part VII Late Phases of Stellar Evolution 34 Evolution on the Asymptotic Giant Branch 417 341 Nuclear Shells on the Asymptotic Giant Branch417 342 Shell Sources and Their Stability419 343 Thermal Pulses of a Shell Source422 344 The Core-Mass-Luminosity Relation for Large Core Masses 424 345 Nucleosynthesis on the AGB 426 346 Mass Loss on the AGB 430 347 A Sample AGB Evolution433 348 Super-AGB Stars 436 349 Post-AGB Evolution 438 35 Later Phases of Core Evolution 439 351 Nuclear Cycles439 352 Evolution of the Central Region441 36 Final Explosions and Collapse 449 361 The Evolution of the CO-Core 450 362 Carbon Ignition in Degenerate Cores454 3621 The Carbon Flash 454 3622 Nuclear Statistical Equilibrium 455 3623 Hydrostatic and Convective Adjustment 458 3624 Combustion Fronts 459 3625 Carbon Burning in AccretingWhite Dwarfs 461 363 Collapse of Cores of Massive Stars 461 3631 Simple Collapse Solutions 462 3632 The Reflection of the Infall 465 3633 Effects of Neutrinos 466 3634 Electron-Capture Supernovae 469 3635 Pair-Creation Instability469 364 The Supernova-Gamma-Ray-Burst Connection 471 Part VIII Compact Objects 37 White Dwarfs 475 371 Chandrasekhar's Theory475 372 The Corrected Mechanical Structure 479 3721 Crystallization 480 3722 Pycnonuclear Reactions482 3723 Inverse ˇ Decays483 3724 Nuclear Equilibrium483 373 Thermal Properties and Evolution of White Dwarfs487 38 Neutron Stars 497 381 Cold Matter Beyond Neutron Drip 497 382 Models of Neutron Stars 501 39 Black Holes509 Part IX Pulsating Stars 40 Adiabatic Spherical Pulsations 519 401 The Eigenvalue Problem 519 402 The Homogeneous Sphere 523 403 Pulsating Polytropes 525 41 Non-adiabatic Spherical Pulsations529 411 Vibrational Instability of the Piston Model 529 412 The Quasi-adiabatic Approximation 531 413 The Energy Integral 532 4131 The _ Mechanism 534 4132 The " Mechanism 534 414 Stars Driven by the _ Mechanism: The Instability Strip535 415 Stars Driven by the " Mechanism541 42 Non-radial Stellar Oscillations 543 421 Perturbations of the Equilibrium Model 543 422 Normal Modes and Dimensionless Variables 545 423 The Eigenspectra548 424 Stars Showing Non-radial Oscillations 552 Part X Stellar Rotation 43 The Mechanics of Rotating Stellar Models557 431 Uniformly Rotating Liquid Bodies 557 432 The Roche Model 560 433 Slowly Rotating Polytropes 562 44 The Thermodynamics of Rotating Stellar Models565 441 Conservative Rotation565 442 Von Zeipel's Theorem566 443 Meridional Circulation 567 444 The Non-conservative Case 569 445 The Eddington-Sweet Timescale570 446 Meridional Circulation in Inhomogeneous Stars573 45 The Angular-Velocity Distribution in Stars 575 451 Viscosity

基彭汉(R. Kippenhahn)，德国哥廷根教授。

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