中外物理学精品书系：恒星结构与演化（第二版 英文影印版）

图书标准信息

• 作者 [德]基彭汉（R. Kippenhahn）、[德]基彭汉（R. Kippenhahn） 著
• 出版社 北京大学出版社
• 出版时间 2014-12
• 版次 1
• ISBN 9787301251751
• 定价 106.00元
• 装帧 平装
• 开本 16开
• 纸张 胶版纸
• 页数 628页
• 字数 748千字
• 丛书 中外物理学精品书系

【内容简介】

　　《中外物理学精品书系：恒星结构与演化（第二版 英文影印版）》详细地介绍了恒星的结构和演化理论。从恒星的组成成分讲起，讲解了恒星中的热核反应过程、热核反应之后的产物、超新星爆发等等一系列想象和理论。对于白矮星、中子星和黑洞也都做了详细介绍。本书适合天体物理方向的科研工作者和研究生阅读。

【作者简介】

　　基彭汉（R. Kippenhahn），德国哥廷根教授。

【目录】

PartITheBasicEquations
1Coordinates，MassDistribution，andGravitationalField
inSphericalStars...........................................................3
1.1EulerianDescription................................................3
1.2LagrangianDescription.............................................4
1.3TheGravitationalField.............................................6

2ConservationofMomentum...............................................9
2.1HydrostaticEquilibrium............................................9
2.2TheRoleofDensityandSimpleSolutions........................10
2.3SimpleEstimatesofCentralValuesPc;Tc........................12
2.4TheEquationofMotionforSphericalSymmetry.................13
2.5TheNon-sphericalCase............................................15
2.6HydrostaticEquilibriuminGeneralRelativity....................15
2.7ThePistonModel...................................................17

3TheVirialTheorem........................................................19
3.1StarsinHydrostaticEquilibrium...................................19
3.2TheVirialTheoremofthePistonModel..........................21
3.3TheKelvin-HelmholtzTimescale.................................22
3.4TheVirialTheoremforNon-vanishingSurfacePressure.........23

4ConservationofEnergy....................................................25
4.1ThermodynamicRelations..........................................25
4.2ThePerfectGasandtheMeanMolecularWeight.................28
4.3ThermodynamicQuantitiesforthePerfect，MonatomicGas.....30
4.4EnergyConservationinStars.......................................31
4.5GlobalandLocalEnergyConservation............................33
4.6Timescales...........................................................35

5TransportofEnergybyRadiationandConduction....................37
5.1RadiativeTransportofEnergy.....................................37
5.1.1BasicEstimates............................................37
5.1.2DiffusionofRadiativeEnergy............................38
5.1.3TheRosselandMeanfor__...............................40
5.2ConductiveTransportofEnergy...................................42
5.3TheThermalAdjustmentTimeofaStar..........................43
5.4ThermalPropertiesofthePistonModel...........................45

6StabilityAgainstLocal，Non-sphericalPerturbations..................47
6.1DynamicalInstability...............................................47
6.2OscillationofaDisplacedElement................................52
6.3VibrationalStability................................................54
6.4TheThermalAdjustmentTime.....................................55
6.5SecularInstability...................................................56
6.6TheStabilityofthePistonModel..................................58

7TransportofEnergybyConvection......................................61
7.1TheBasicPicture...................................................62
7.2DimensionlessEquations...........................................65
7.3LimitingCases，Solutions，Discussion.............................66
7.4ExtensionsoftheMixing-LengthTheory.........................70

8TheChemicalComposition................................................73
8.1RelativeMassAbundances.........................................73
8.2VariationofCompositionwithTime...............................74
8.2.1RadiativeRegions.........................................74
8.2.2Diffusion...................................................76
8.2.3ConvectiveRegions.......................................80

9MassLoss....................................................................83
PartIITheOverallProblem

10TheDifferentialEquationsofStellarEvolution.........................89
10.1TheFullSetofEquations..........................................89
10.2TimescalesandSimplifications....................................91

11BoundaryConditions......................................................93
11.1CentralConditions..................................................93
11.2SurfaceConditions..................................................95
11.3InfluenceoftheSurfaceConditionsandPropertiesof
EnvelopeSolutions.................................................98
11.3.1RadiativeEnvelopes.......................................98
11.3.2ConvectiveEnvelopes.....................................101
11.3.3Summary..................................................102
11.3.4TheT_rStratification....................................102

12NumericalProcedure.......................................................105
12.1TheShootingMethod...............................................105
12.2TheHenyeyMethod................................................106
12.3TreatmentoftheFirst-andSecond-OrderTimeDerivatives.....113
12.4TreatmentoftheDiffusionEquation...............................115
12.5TreatmentofMassLoss............................................117
12.6ExistenceandUniqueness..........................................118
PartIIIPropertiesofStellarMatter

13ThePerfectGaswithRadiation...........................................123
13.1RadiationPressure..................................................123
13.2ThermodynamicQuantities.........................................124

14Ionization....................................................................127
14.1TheBoltzmannandSahaFormulae................................127
14.2IonizationofHydrogen.............................................130
14.3ThermodynamicalQuantitiesforaPureHydrogenGas..........132
14.4Hydrogen-HeliumMixtures........................................133
14.5TheGeneralCase...................................................135
14.6LimitationoftheSahaFormula....................................137

15TheDegenerateElectronGas.............................................139
15.1ConsequencesofthePauliPrinciple...............................139
15.2TheCompletelyDegenerateElectronGas.........................140
15.3LimitingCases......................................................144
15.4PartialDegeneracyoftheElectronGas............................145

16TheEquationofStateofStellarMatter..................................151
16.1TheIonGas.........................................................151
16.2TheEquationofState...............................................152
16.3ThermodynamicQuantities.........................................154
16.4Crystallization.......................................................157
16.5Neutronization......................................................158
16.6RealGasEffects....................................................159

17Opacity.......................................................................163
17.1ElectronScattering..................................................163
17.2AbsorptionDuetoFree-FreeTransitions.........................164
17.3Bound-FreeTransitions............................................165
17.4Bound-BoundTransitions..........................................166
17.5TheNegativeHydrogenIon........................................168
17.6Conduction..........................................................169
17.7MolecularOpacities................................................170
17.8OpacityTables......................................................172

18NuclearEnergyProduction...............................................175
18.1BasicConsiderations................................................175
18.2NuclearCrossSections.............................................179
18.3ThermonuclearReactionRates.....................................182
18.4ElectronShielding..................................................188
18.5TheMajorNuclearBurningStages................................192
18.5.1HydrogenBurning........................................193
18.5.2HeliumBurning...........................................197
18.5.3CarbonBurningandBeyond.............................199
18.6Neutron-CaptureNucleosynthesis.................................201
18.7Neutrinos............................................................205
PartIVSimpleStellarModels

19PolytropicGaseousSpheres...............................................213
19.1PolytropicRelations................................................213
19.2PolytropicStellarModels..........................................215
19.3PropertiesoftheSolutions.........................................216
19.4ApplicationtoStars.................................................218
19.5RadiationPressureandthePolytropenD3......................219
19.6PolytropicStellarModelswithFixedK...........................220
19.7Chandrasekhar'sLimitingMass....................................221
19.8IsothermalSpheresofanIdealGas................................222
19.9GravitationalandTotalEnergyforPolytropes....................224
19.10SupermassiveStars.................................................226
19.11ACollapsingPolytrope.............................................227

20HomologyRelations........................................................233
20.1DefinitionsandBasicRelations....................................233
20.2ApplicationstoSimpleMaterialFunctions........................237
20.2.1TheCase?D0............................................237
20.2.2TheCase?D?D'D1;aDbD0...................237
20.2.3TheRoleoftheEquationofState........................239
20.3HomologousContraction...........................................241

21SimpleModelsintheU-VPlane.........................................243
21.1TheU-VPlane.....................................................243
21.2RadiativeEnvelopeSolutions......................................246
21.3FittingofaConvectiveCore........................................248
21.4FittingofanIsothermalCore.......................................250

22TheZero-AgeMainSequence.............................................251
22.1SurfaceValues......................................................251
22.2InteriorSolutions...................................................254
22.3ConvectiveRegions.................................................258
22.4ExtremeValuesofM...............................................260
22.5TheEddingtonLuminosity.........................................261

23OtherMainSequences.....................................................263
23.1TheHeliumMainSequence........................................263
23.2TheCarbonMainSequence........................................266
23.3GeneralizedMainSequences.......................................267

24TheHayashiLine...........................................................271
24.1LuminosityofFullyConvectiveModels...........................272
24.2ASimpleDescriptionoftheHayashiLine........................273
24.3TheNeighbourhoodoftheHayashiLine
andtheForbiddenRegion..........................................276
24.4NumericalResults..................................................279
24.5LimitationsforFullyConvectiveModels..........................281

25StabilityConsiderations...................................................283
25.1GeneralRemarks....................................................283
25.2StabilityofthePistonModel.......................................285
25.2.1DynamicalStability.......................................285
25.2.2InclusionofNon-adiabaticEffects.......................286
25.3StellarStability......................................................288
25.3.1PerturbationEquations....................................289
25.3.2DynamicalStability.......................................290
25.3.3Non-adiabaticEffects.....................................292
25.3.4TheGravothermalSpecificHeat.........................293
25.3.5SecularStabilityBehaviourofNuclearBurning........294
PartVEarlyStellarEvolution

26TheOnsetofStarFormation..............................................299
26.1TheJeansCriterion.................................................299
26.1.1AnInfiniteHomogeneousMedium......................299
26.1.2APlane-ParallelLayerinHydrostaticEquilibrium.....302
26.2InstabilityintheSphericalCase....................................303
26.3Fragmentation.......................................................307

27TheFormationofProtostars..............................................311
27.1Free-FallCollapseofaHomogeneousSphere....................311
27.2CollapseontoaCondensedObject.................................313
27.3ACollapseCalculation.............................................314
27.4TheOpticallyThinPhaseandtheFormation
ofaHydrostaticCore...............................................315
27.5CoreCollapse.......................................................317
27.6EvolutionintheHertzsprung-RussellDiagram...................320

28Pre-Main-SequenceContraction..........................................323
28.1HomologousContractionofaGaseousSphere....................323
28.2ApproachtotheZero-AgeMainSequence........................326

29FromtheInitialtothePresentSun.......................................329
29.1KnownSolarData..................................................329
29.2ChoosingtheInitialModel.........................................331
29.3AStandardSolarModel............................................333
29.4ResultsofHelioseismology........................................336
29.5SolarNeutrinos......................................................338

30EvolutionontheMainSequence..........................................343
30.1ChangeintheHydrogenContent..................................343
30.2EvolutionintheHertzsprung-RussellDiagram...................346
30.3TimescalesforCentralHydrogenBurning........................347
30.4ComplicationsConnectedwithConvection.......................348
30.4.1ConvectiveOvershooting.................................349
30.4.2Semiconvection............................................354
30.5TheSch¨onberg-ChandrasekharLimit......................