Stellar Physics - 2: Stellar Evolution and Stability

Stellar Physics

Preface to the Second English Edition

Preface to the First English Edition

Preface to the Russian Edition

Contents of Volume 1

Contents of Volume 2

7 Star Formation

7.1 Observations of the Regions of Star Formation

7.1.1 Introduction

7.1.2 Observational Data

7.2 Spherically Symmetric Collapseof Interstellar Clouds

7.2.1 Heat Balance of an Optically Thin Cloud

7.2.2 Equations for Cloud Collapse

7.2.3 Calculational Results

7.3 Collapse of Rotating Clouds

7.3.1 Set of Equations and Difference Scheme Properties

7.3.2 Calculational Results

8 Pre-Main Sequence Evolution

8.1 Hayashi Phase

8.1.1 Nuclear Reactions

8.1.2 Non-Ideality of Matter

8.1.3 Evolution of Low-Mass Stars, Minimum Mass of a Star on the Main Sequence, Role of Various Factors

8.1.4 Evolutionary Role of the Mass Loss

8.2 Evolution of Rapidly Rotating Stars on Gravitational Contraction Stages

8.2.1 On the Distribution of Angular Velocity of Rotation

8.2.2 Method for Evolutionary Calculations

8.2.3 Calculation Results

8.3 Models for the Matter Outflow from Young Stars

8.3.1 Outflowing Bipolytropic Models

8.3.2 Outflowing Models for Isentropic Hydrogen Stars

8.3.3 Models for Outflowing Coronae of Young Stars

8.3.4 On the Phenomenon of Fuor

9 Nuclear Evolution of Stars

9.1 Sources of Uncertainty in Evolutionary Calculations

9.1.1 Convection

9.1.2 Semiconvection

9.1.3 Convective Non-Locality and Overshooting

9.1.4 Opacity and Nuclear Reactions

9.1.5 Methods for Calculating Envelope

9.1.6 Other Factors

9.2 Evolution of Stars in Quiescent Burning Phases

9.2.1 Iben's Calculations

9.2.2 Paczynski's Calculations

9.2.3 Evolution of Massive Stars

9.2.4 Evolution of Massive Stars with Mass Loss

9.2.5 CAK Theory

9.2.6 Line-Driven Winds in the Presence of Strong Gravitational Fields

9.2.7 Calculations with New Opacity Tables

9.3 Evolution with Degeneracy, Thermal Flashes

9.3.1 Core Helium Flash

9.3.2 Horizontal Branch

9.3.3 Asymptotic Giant Branch

9.3.4 Thermal Flashes in Helium-Burning Shell

9.3.5 The Mass Loss in AGB Stars

9.3.6 Evolution with Mass Loss: From AGB to White Dwarf State

9.3.7 On Mixing on the AGB and in Neighbourhoods

9.3.8 Thermal Instability in Degenerate Carbon Core

9.3.9 Convective ²URCA Shells²

9.3.9.1 Energy Equation in Presence of the Convective URCA Shell

9.3.9.2 Convective Flux

10 Collapse and Supernovae

10.1 Presupernova Models

10.1.1 Stellar Cores at Threshold of Hydrodynamical Stability: Energetic Method

10.1.2 Stellar Cores at Thermal Instability Threshold

10.2 Explosions Resulting from the Thermal Instability Development in Degenerate Carbon Cores

10.2.1 Basic Equations

10.2.2 Detonation

10.2.3 Deflagration

10.2.4 Spontaneous Burning and Detonation

10.2.5 Instabilities of Nuclear Flames

10.3 Collapse of Low-Mass Stellar Cores

10.4 Hydrodynamical Collapse of Stellar Cores

10.4.1 Low-Energy Window for Neutrinos

10.4.2 Asymmetric Neutrino Emission During Collapse of a Star with a Strong Magnetic Field

10.4.3 Neutrino Oscillations in Matter

10.4.4 Convective Instability in Collapsing Stellar Cores

10.4.5 Two-Dimensional and Three-Dimensional Calculations of Neutrino Convection

10.4.6 Explosion of Rapidly Rotating Star

10.4.7 Standing Accretion Induced Instability

10.4.8 Acoustic Explosion Model

10.5 Magnetorotational Model of Supernova Explosion

10.5.1 Mechanism of Magnetorotational Explosion

10.5.2 Basic Equations

10.5.3 Cylindrical Approximation

10.5.4 Calculational Results

10.5.5 Two-Dimensional Numerical Method in MHD

10.5.6 Magnetorotational Explosion of the Initially Uniform Cloud

10.5.7 Magnetorotational Supernova: Quadruple and Dipole Magnetic Configurations

10.5.8 Development of the Magnetorotational Instability in 2D Simulations

10.5.9 Symmetry Breaking Of the Magnetic Field, Anisotropic Neutrino Emission and High Velocity Neutron Star Formation

10.5.10 A Kick Due to Hydrodynamic Instabilities

11 Final Stages of Stellar Evolution

11.1 White Dwarfs

11.1.1 Case T=0

11.1.2 Account for a Finite Value of T and Cooling

11.1.3 Cooling of White Dwarfs Near the Stability Limit with the Inclusion of Heating by Non-Equilibrium -Processes [34]

11.1.4 On the Evolution of Magnetic Fields in White Dwarfs

11.1.5 Nova Outbursts

11.2 Neutron Stars

11.2.1 Cold Neutron Stars

11.2.2 Hot Neutron Stars

11.2.3 Cooling of Neutron Stars

11.2.4 Magnetic Field Decay in Neutron Stars

11.2.5 Stars with Neutron Cores

11.2.6 Quark stars

11.2.6.1 Strange Quark Matter

11.2.6.2 Strange Stars

11.2.6.3 The Surface: Bare or Crusted Strange Stars?

11.3 Black Holes and Accretion

11.3.1 Spherically Symmetric Accretion

11.3.2 Accretion at an Ordered Magnetic Field

11.3.3 Conical Accretion on to a Rapidly Moving Black Hole

11.3.4 Disk Accretion in Binaries

11.3.5 Accretion Disc Structure with Optically Thin/Thick Transition

11.3.6 Black Hole Advective Accretion Disks with Optical Depth Transition

11.3.6.1 Basic Equations

11.3.6.2 Singular Points and Uniqueness of Solutions

11.3.6.3 Method of Solution

11.3.6.4 Numerical Results and Physical Effects

11.3.7 Large-Scale Magnetic Fields Dragging in Accretion Disks

11.3.7.1 Turbulent Disk with Radiative Outer Zones

11.3.8 Battery Effect in Accretion Disks

11.3.8.1 Radiatively Induced Current and Toroidal Magnetic Field Production in Accretion Disks

11.3.8.2 Production of a Poloidal Magnetic Field in Optically Thin Accretion Flows by Poynting--Robertson Effect

11.3.9 Screening of the Magnetic Field of Disk Accreting Stars

11.3.10 Jet Confinement by Magneto-Torsional Oscillations

11.3.10.1 Profiling in Axially Symmetric MHD Equations

11.3.10.2 Further Simplification: Reducing the Problem to an Ordinary Differential Equation

11.3.10.3 Numerical Solution

11.3.10.4 Restrictions of the Model

11.4 Cosmic Gamma Ray Bursts: Observations and Modeling

11.4.1 Central Engine of Cosmic Gamma-Ray Bursts

11.4.2 Optical Afterglows

11.4.3 Short GRB and Giant SGR Bursts

11.4.4 High Energy Afterglows (30--10,000MeV)

12 Dynamic Stability

12.1 Hierarchy of Time Scales

12.2 Variational Principle and Small Perturbations

12.2.1 Variational Principle in General Relativity

12.2.2 Newtonian and Post-Newtonian Limits

12.2.3 Method of Small Perturbations in Newtonian Theory

12.3 Static Criteria for Stability

12.3.1 Non-Rotating Stars

12.3.2 Criteria for Rotating Stars

12.3.3 Removal of Degeneracy of Neutral Oscillatory Modes in Rotating Isentropic Stars

12.3.4 Numerical Examples

12.4 Star Stability in the Presence of a Phase Transition

12.4.1 Evaluation of Variations and 2

12.4.2 Other Forms of Stability Criterion

12.4.3 Rough Test for Stability

12.4.4 Derivation of Stability Condition for a Phase Transition in the Center of Star

12.5 Dynamic Stabilization of NonSpherical Bodies Against Unlimited Collapse

12.5.1 Equations of Motion

12.5.2 Dimensionless Equations

12.5.3 Numerical Results for the Case H=0

12.5.4 Poincaré Section

12.5.4.1 The Bounding Curve

12.6 General Picture

13 Thermal Stability

13.1 Evolutionary Phases Exhibiting Thermal Instabilities

13.1.1 Instability in Degenerate Regions

13.1.2 Instabilities in the Absence of Degeneracy

13.2 Thermal Instability Development in Non-Degenerate Shells

13.2.1 Stability of a Burning Shell with Constant Thickness

13.2.2 Calculations of Density Perturbations

13.2.3 A Strict Criterion for Thermal Stability

14 Stellar Pulsations and Stability

14.1 Eigenmodes

14.1.1 Equations for Small Oscillations

14.1.2 Boundary Conditions

14.1.3 p-, g- and f-Modes

14.1.4 Pulsational Instability

14.2 Pulsations in Stars with Phase Transition

14.2.1 Equations of Motion in the Presence of a Phase Transition

14.2.2 Physical Processes at the Phase Jump

14.2.3 Adiabatic Oscillations of Finite Amplitude

14.2.4 Decaying Finite-Amplitude Oscillations

14.3 Pulsational Stability of Massive Stars

14.3.1 The Linear Analysis

14.3.2 Non-Linear Oscillations

14.4 On Variable Stars and Stellar Seismology

References

List of Symbols and Abbreviations

Some Important Constants

Subject Index