Stars and Stellar Processes 1st Edition by Mike Guidry 1107197880 9781107197886

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ISBN-10 :  1107197880 

ISBN-13 :  9781107197886

Author:  Mike Guidry 

This textbook offers a modern approach to the physics of stars, assuming only undergraduate-level preparation in mathematics and physics, and minimal prior knowledge of astronomy. It starts with a concise review of introductory concepts in astronomy, before covering the nuclear processes and energy transport in stellar interiors, and stellar evolution from star formation to the common stellar endpoints as white dwarfs and neutron stars. In addition to the standard material, the author also discusses more contemporary topics that students will find engaging, such as neutrino oscillations and the MSW resonance, supernovae, gamma-ray bursts, advanced nucleosynthesis, neutron stars, black holes, cosmology, and gravitational waves. With hundreds of worked examples, explanatory boxes, and problems with solutions, this textbook provides a solid foundation for learning either in a classroom setting or through self-study.

Stars and Stellar Processes 1st Table of contents:

Part I Stellar Structure
1 Some Properties of Stars
1.1 Luminosities and Magnitudes
1.1.1 Stellar Luminosities
1.1.2 Photon Luminosities
1.1.3 Apparent Magnitudes
1.1.4 The Parsec Distance Unit
1.1.5 Absolute Magnitudes
1.1.6 Bolometric Magnitudes
1.2 Stars as Blackbody Radiators
1.2.1 Radiation Laws
1.2.2 Effective Temperatures
1.2.3 Stellar Radii from Effective Temperatures
1.3 Color Indices
1.4 Masses and Physical Radii of Stars
1.5 Binary Star Systems
1.5.1 Motion of Binary Systems
1.5.2 Radial Velocities and Masses
1.5.3 True Orbit for Visual Binaries
1.5.4 Eclipsing Binaries
1.6 Mass–Luminosity Relationships
1.7 Summary of Physical Quantities for Stars
1.8 Proper Motion and Space Velocities
1.9 Stellar Populations
1.9.1 Population I and Population II
1.9.2 Population III
1.10 Variable Stars and Period–Luminosity Relations
1.10.1 Cepheid Variables
1.10.2 RR Lyra Variables
1.10.3 Pulsational Instabilities
1.10.4 Pulsations and Free-Fall Timescales
Background and Further Reading
Problems
2 The Hertzsprung–Russell Diagram
2.1 Spectral Classes
2.1.1 Excitation and the Boltzmann Formula
2.1.2 Ionization and the Saha Equations
2.1.3 Ionization of Hydrogen and Helium
2.1.4 Optimal Temperatures for Spectral Lines
2.1.5 The Spectral Sequence
2.2 HR Diagram for Stars Near the Sun
2.2.1 Solving the Distance Problem
2.2.2 Features of the HR Diagram
2.3 HR Diagram for Clusters
2.4 Luminosity Classes
2.4.1 Pressure Broadening of Spectral Lines
2.4.2 Inferring Luminosity Class from Surface Density
2.5 Spectroscopic Parallax
2.6 The HR Diagram and Stellar Evolution
Background and Further Reading
Problems
3 Stellar Equations of State
3.1 Equations of State
3.2 The Pressure Integral
3.3 Ideal Gas Equation of State
3.3.1 Internal Energy
3.3.2 The Adiabatic Index
3.4 Mean Molecular Weights
3.4.1 Concentration Variables
3.4.2 Partially Ionized Gases
3.4.3 Fully-Ionized Gases
3.4.4 Shorthand Notation and Approximations
3.5 Polytropic Equations of State
3.5.1 Polytropic Processes
3.5.2 Properties of Polytropes
3.6 Adiabatic Equations of State
3.7 Equations of State for Degenerate Gases
3.7.1 Pressure Ionization
3.7.2 Distinguishing Classical and Quantum Gases
3.7.3 Nonrelativistic Classical and Quantum Gases
3.7.4 Ultrarelativistic Classical and Quantum Gases
3.7.5 Transition from a Classical to Quantum Gas
3.8 The Degenerate Electron Gas
3.8.1 Fermi Momentum and Fermi Energy
3.8.2 Equation of State for Nonrelativistic Electrons
3.8.3 Equation of State for Ultrarelativistic Electrons
3.9 High Gas Density and Stellar Structure
3.10 Equation of State for Radiation
3.11 Matter and Radiation Mixtures
3.11.1 Mixtures of Ideal Gases and Radiation
3.11.2 Adiabatic Systems of Gas and Radiation
3.11.3 Radiation and Gravitational Stability
Background and Further Reading
Problems
4 Hydrostatic and Thermal Equilibrium
4.1 Newtonian Gravitation
4.2 Conditions for Hydrostatic Equilibrium
4.3 Lagrangian and Eulerian Descriptions
4.3.1 Lagrangian Formulation of Hydrostatics
4.3.2 Contrasting Lagrangian and Eulerian Descriptions
4.4 Dynamical Timescales
4.5 The Virial Theorem for an Ideal Gas
4.6 Thermal Equilibrium
4.7 Total Energy for a Star
4.8 Stability and Heat Capacity
4.8.1 Temperature Response to Energy Fluctuations
4.8.2 Heating Up while Cooling Down
4.9 The Kelvin–Helmholtz Timescale
Background and Further Reading
Problems
5 Thermonuclear Reactions in Stars
5.1 Nuclear Energy Sources
5.1.1 The Curve of Binding Energy
5.1.2 Masses and Mass Excesses
5.1.3 Q-Values
5.1.4 Efficiency of Hydrogen Burning
5.2 Thermonuclear Hydrogen Burning
5.2.1 The Proton–Proton Chains
5.2.2 The CNO Cycle
5.2.3 Competition of PP Chains and the CNO Cycle
5.3 Cross Sections and Reaction Rates
5.3.1 Reaction Cross Sections
5.3.2 Rates from Cross Sections
5.4 Thermally Averaged Reaction Rates
5.5 Parameterization of Cross Sections
5.6 Nonresonant Cross Sections
5.6.1 Coulomb Barriers
5.6.2 Barrier Penetration Factors
5.6.3 Astrophysical S-Factors
5.6.4 The Gamow Window
5.7 Resonant Cross Sections
5.8 Calculations with Rate Libraries
5.9 Total Rate of Energy Production
5.10 Temperature and Density Exponents
5.11 Neutron Reactions and Weak Interactions
5.12 Reaction Selection Rules
5.12.1 Angular Momentum Conservation
5.12.2 Isotopic Spin Conservation
5.12.3 Parity Conservation
Background and Further Reading
Problems
6 Stellar Burning Processes
6.1 Reactions of the Proton–Proton Chains
6.1.1 Reactions of PP-I
6.1.2 Branching for PP-II and PP-III
6.1.3 Effective Q-Values
6.2 Reactions of the CNO Cycle
6.2.1 The CNO Cycle in Operation
6.2.2 Rate of CNO Energy Production
6.3 The Triple-α Process
6.3.1 Equilibrium Population of 8Be
6.3.2 Formation of the Excited State in [sup(12)]C
6.3.3 Formation of the Ground State in [sup(12)]C
6.3.4 Energy Production in the Triple-α Reaction
6.4 Helium Burning to C, O, and Ne
6.4.1 Oxygen and Neon Production
6.4.2 The Outcome of Helium Burning
6.5 Advanced Burning Stages
6.5.1 Carbon, Oxygen, and Neon Burning
6.5.2 Silicon Burning
6.6 Timescales for Advanced Burning
Background and Further Reading
Problems
7 Energy Transport in Stars
7.1 Modes of Energy Transport
7.2 Diffusion of Energy
7.3 Energy Transport by Conduction
7.4 Radiative Energy Transport
7.4.1 Thomson Scattering
7.4.2 Conduction in Degenerate Matter
7.4.3 Absorption of Photons
7.4.4 Stellar Opacities
7.4.5 General Contributions to Stellar Opacity
7.5 Energy Transport by Convection
7.6 Conditions for Convective Instability
7.6.1 The Schwarzschild Instability
7.6.2 The Ledoux Instability
7.6.3 Salt-Finger Instability
7.7 Critical Temperature Gradient for Convection
7.7.1 Convection and the Adiabatic Index
7.7.2 Convection and the Pressure Gradient
7.8 Stellar Temperature Gradients
7.8.1 Choice between Radiative or Convective Transport
7.8.2 Radiative Temperature Gradients
7.9 Mixing-Length Treatment of Convection
7.9.1 Pressure Scale Height
7.9.2 The Mixing-Length Philosophy
7.9.3 Analysis of Solar Convection
7.10 Examples of Stellar Convective Regions
7.10.1 Convection in Stellar Cores
7.10.2 Surface Ionization Zones
7.11 Energy Transport by Neutrino Emission
7.11.1 Neutrino Production Mechanisms
7.11.2 Classification and Rates
7.11.3 Coherent Neutrino Scattering
Background and Further Reading
Problems
8 Summary of Stellar Equations
8.1 The Basic Equations Governing Stars
8.1.1 Hydrostatic Equilibrium
8.1.2 Luminosity
8.1.3 Temperature Gradient
8.1.4 Changes in Isotopic Composition
8.1.5 Equation of State
8.2 Solution of the Stellar Equations
8.3 Important Stellar Timescales
8.4 Hydrostatic Equilibrium for Polytropes
8.4.1 Lane–Emden Equation and Solutions
8.4.2 Computing Physical Quantities
8.4.3 Limitations of the Lane–Emden Approximation
8.5 Numerical Solution of the Stellar Equations
Background and Further Reading
Problems
Part II Stellar Evolution
9 The Formation of Stars
9.1 Evidence for Starbirth in Nebulae
9.2 Jeans Criterion for Gravitational Collapse
9.3 Fragmentation of Collapsing Clouds
9.4 Stability in Adiabatic Approximation
9.4.1 Dependence on Adiabatic Exponents
9.4.2 Physical Interpretation
9.5 The Collapse of a Protostar
9.5.1 Initial Free-Fall Collapse
9.5.2 A Little More Realism
9.6 Onset of Hydrostatic Equilibrium
9.7 Termination of Fragmentation
9.8 Hayashi Tracks
9.8.1 Fully Convective Stars
9.8.2 Development of a Radiative Core
9.8.3 Dependence on Composition and Mass
9.9 Limiting Lower Mass for Stars
9.10 Brown Dwarfs
9.10.1 Spectroscopic Signatures
9.10.2 Stars, Brown Dwarfs, and Planets
9.11 Limiting Upper Mass for Stars
9.11.1 Eddington Luminosity
9.11.2 Estimate of Upper Limiting Mass
9.12 The Initial Mass Function
9.13 Protoplanetary Disks
9.14 Exoplanets
9.14.1 The Doppler Spectroscopy Method
9.14.2 Transits of Extrasolar Planets
Background and Further Reading
Problems
10 Life and Times on the Main Sequence
10.1 The Standard Solar Model
10.1.1 Composition of the Sun
10.1.2 Energy Generation and Composition Changes
10.1.3 Hydrostatic Equilibrium
10.1.4 Energy Transport
10.1.5 Constraints and Solution
10.2 Helioseismology
10.2.1 Solar p-Modes and g-Modes
10.2.2 Surface Vibrations and the Solar Interior
10.3 Solar Neutrino Production
10.3.1 Sources of Solar Neutrinos
10.3.2 Testing the Standard Solar Model with Neutrinos
10.4 The Solar Electron-Neutrino Deficit
10.4.1 The Davis Chlorine Experiment
10.4.2 The Gallium Experiments
10.4.3 Super Kamiokande
10.4.4 Astrophysics and Particle Physics Explanations
10.5 Evolution of Stars on the Main Sequence
10.6 Timescale for Main Sequence Lifetimes
10.7 Evolutionary Timescales
10.8 Evolution Away from the Main Sequence
10.8.1 Three Categories of Post Main Sequence Evolution
10.8.2 Examples of Post Main Sequence Evolution
Background and Further Reading
Problems
11 Neutrino Flavor Oscillations
11.1 Overview of the Solar Neutrino Problem
11.2 Weak Interactions and Neutrino Physics
11.2.1 Matter and Force Fields of the Standard Model
11.2.2 Masses for Particles of the Standard Model
11.2.3 Charged and Neutral Currents
11.3 Flavor Mixing
11.3.1 Flavor Mixing in the Quark Sector
11.3.2 Flavor Mixing in the Leptonic Sector
11.4 Implications of a Finite Neutrino Mass
11.5 Neutrino Vacuum Oscillations
11.5.1 Mixing for Two Neutrino Flavors
11.5.2 The Vacuum Oscillation Length
11.5.3 Time-Averaged or Classical Probabilities
11.6 Neutrino Oscillations with Three Flavors
11.6.1 CP Violation in Neutrino Oscillations
11.6.2 The Neutrino Mass Hierarchy
11.6.3 Recovering 2-Flavor Mixing
11.7 Neutrino Masses and Particle Physics
Background and Further Reading
Problems
12 Solar Neutrinos and the MSW Effect
12.1 Propagation of Neutrinos in Matter
12.1.1 Matrix Elements for Interaction with Matter
12.1.2 The Effective Neutrino Mass in Medium
12.2 The Mass Matrix
12.2.1 Propagation of Left-Handed Neutrinos
12.2.2 Evolution in the Flavor Basis
12.2.3 Propagation in Matter
12.3 Solutions in Matter
12.3.1 Mass Eigenvalues for Constant Density
12.3.2 The Matter Mixing Angle θ[sub(m)]12.3.3 The Matter Oscillation Length L[sub(m)]12.3.4 Flavor Conversion in Constant-Density Matter
12.4 The MSW Resonance Condition
12.5 Resonant Flavor Conversion
12.6 Propagation in Matter of Varying Density
12.7 The Adiabatic Criterion
12.8 MSW Neutrino Flavor Conversion
12.8.1 Flavor Conversion in Adiabatic Approximation
12.8.2 Adiabatic Conversion and the Mixing Angle
12.8.3 Resonant Conversion for Large or Small θ
12.8.4 Energy Dependence of Flavor Conversion
12.9 Resolution of the Solar Neutrino Problem
12.9.1 Super-K Observation of Flavor Oscillation
12.9.2 SNO Observation of Neutral Current Interactions
12.9.3 KamLAND Constraints on Mixing Angles
12.9.4 Large Mixing Angles and the MSW Mechanism
12.9.5 A Tale of Large and Small Mixing Angles
Background and Further Reading
Problems
13 Evolution of Lower-Mass Stars
13.1 Endpoints of Stellar Evolution
13.2 Shell Burning
13.3 Stages of Red Giant Evolution
13.4 The Red Giant Branch
13.4.1 The Schönberg–Chandrasekhar Limit
13.4.2 Crossing the Hertzsprung Gap
13.5 Helium Ignition
13.5.1 Core Equation of State and Helium Ignition
13.5.2 Thermonuclear Runaways in Degenerate Matter
13.5.3 The Helium Flash
13.6 Horizontal Branch Evolution
13.6.1 Life on the Helium Main Sequence
13.6.2 Leaving the Horizontal Branch
13.7 Asymptotic Giant Branch Evolution
13.7.1 Thermal Pulses
13.7.2 Slow Neutron Capture
13.7.3 Development of Deep Convective Envelopes
13.7.4 Mass Loss
13.8 Ejection of the Envelope
13.9 White Dwarfs and Planetary Nebulae
13.10 Stellar Dredging Operations
13.11 The Sun’s Red Giant Evolution
13.12 Overview for Low-Mass Stars
Background and Further Reading
Problems
14 Evolution of Higher-Mass Stars
14.1 Unique Features of More Massive Stars
14.2 Advanced Burning Stages in Massive Stars
14.3 Envelope Loss from Massive Stars
14.3.1 Wolf–Rayet Stars
14.3.2 The Strange Case of η Carinae
14.4 Neutrino Cooling of Massive Stars
14.4.1 Local and Nonlocal Cooling
14.4.2 Neutrino Cooling and the Pace of Stellar Evolution
14.5 Massive Population III Stars
14.6 Evolutionary Endpoints for Massive Stars
14.6.1 Observational and Theoretical Characteristics
14.6.2 Black Holes from Failed Supernovae?
14.6.3 Gravitational Waves and Stellar Evolution
14.7 Summary: Evolution after the Main Sequence
14.8 Stellar Lifecycles
Background and Further Reading
Problems
15 Stellar Pulsations and Variability
15.1 The Instability Strip
15.2 Adiabatic Radial Pulsations
15.3 Pulsating Variables as Heat Engines
15.4 Non-adiabatic Radial Pulsations
15.4.1 Thermodynamics of Sustained Pulsation
15.4.2 Opacity and the κ-Mechanism
15.4.3 Partial Ionization Zones and the Instability Strip
15.4.4 The ε-Mechanism and Massive Stars
15.5 Non-radial Pulsation
Background and Further Reading
Problems
16 White Dwarfs and Neutron Stars
16.1 Properties of White Dwarfs
16.1.1 Density and Gravity
16.1.2 Equation of State
16.1.3 Ingredients of a White Dwarf Description
16.2 Polytropic Models of White Dwarfs
16.2.1 Low-Mass White Dwarfs
16.2.2 High-Mass White Dwarfs
16.2.3 Heuristic Derivation of the Chandrasekhar Limit
16.2.4 Effective Adiabatic Index and Gravitational Stability
16.3 Internal Structure of White Dwarfs
16.3.1 Temperature Variation
16.3.2 An Insulating Blanket around a Metal Ball
16.4 Cooling of White Dwarfs
16.5 Crystallization of White Dwarfs
16.6 Beyond White Dwarf Masses
16.7 Basic Properties of Neutron Stars
16.7.1 Sizes and Masses
16.7.2 Internal Structure
16.7.3 Cooling of Neutron Stars
16.7.4 Evidence for Superfluidity in Neutron Stars
16.8 Hydrostatic Equilibrium in General Relativity
16.8.1 The Oppenheimer–Volkov Equations
16.8.2 Comparison with Newtonian Gravity
16.9 Pulsars
16.9.1 The Pulsar Mechanism
16.9.2 Pulsar Magnetic Fields
16.9.3 The Crab Pulsar
16.9.4 Pulsar Spindown and Glitches
16.9.5 Millisecond Pulsars
16.9.6 Binary Pulsars
16.10 Magnetars
Background and Further Reading
Problems
17 Black Holes
17.1 The Failure of Newtonian Gravity
17.2 The General Theory of Relativity
17.2.1 General Covariance
17.2.2 The Principle of Equivalence
17.2.3 Curved Spacetime and Tensors
17.2.4 Curvature and the Strength of Gravity
17.3 Some Important General Relativistic Solutions
17.3.1 The Einstein Equation
17.3.2 Line Elements and Metrics
17.3.3 Minkowski Spacetime
17.3.4 Schwarzschild Spacetime
17.3.5 Kerr Spacetime
17.4 Evidence for Black Holes
17.4.1 Compact Objects in X-ray Binaries
17.4.2 Causality Constraints
17.4.3 The Black Hole Candidate Cygnus X-1
17.5 Black Holes and Gravitational Waves
17.6 Supermassive Black Holes
17.7 Intermediate-Mass and Mini Black Holes
17.8 Proof of the Pudding: Event Horizons
17.9 Some Measured Black Hole Masses
Background and Further Reading
Problems
Part III Accretion, Mergers, and Explosions
18 Accreting Binary Systems
18.1 Classes of Accretion
18.2 Roche-lobe Overflow
18.2.1 The Roche Potential
18.2.2 Lagrange Points
18.2.3 Roche Lobes
18.3 Classification of Binary Star Systems
18.4 Accretion Streams and Accretion Disks
18.4.1 Gas Motion
18.4.2 Initial Accretion Velocity
18.4.3 General Properties of Roche-Overflow Accretion
18.4.4 Disk Dynamics
18.5 Wind-Driven Accretion
18.6 Classification of X-Ray Binaries
18.6.1 High-Mass X-Ray Binaries
18.6.2 Low-Mass X-Ray Binaries
18.6.3 Suppression of Accretion for Intermediate Masses
18.7 Accretion Power
18.7.1 Maximum Energy Release in Accretion
18.7.2 Limits on Accretion Rates
18.7.3 Accretion Temperatures
18.7.4 Maximum Efficiency for Energy Extraction
18.7.5 Storing Energy in Accretion Disks
18.8 Some Accretion-Induced Phenomena
18.9 Accretion and Stellar Evolution
18.9.1 The Algol Paradox
18.9.2 Blue Stragglers
Background and Further Reading
Problems
19 Nova Explosions and X-Ray Bursts
19.1 The Nova Mechanism
19.1.1 The Hot CNO Cycle
19.1.2 Recurrence of Novae
19.1.3 Nucleosynthesis in Novae
19.2 The X-Ray Burst Mechanism
19.2.1 Rapid Proton Capture
19.2.2 Nucleosynthesis and the rp-Process
Background and Further Reading
Problems
20 Supernovae
20.1 Classification of Supernovae
20.1.1 Type Ia
20.1.2 Type Ib and Type Ic
20.1.3 Type II
20.2 Thermonuclear Supernovae
20.2.1 The Single-Degenerate Mechanism
20.2.2 The Double-Degenerate Mechanism
20.2.3 Thermonuclear Burning in Extreme Conditions
20.2.4 Element and Energy Production
20.2.5 Late-Time Observables
20.3 Core Collapse Supernovae
20.3.1 The “Supernova Problem”
20.3.2 The Death of Massive Stars
20.3.3 Sequence of Events in Core Collapse
20.3.4 Neutrino Reheating
20.3.5 Convection and Neutrino Reheating
20.3.6 Convectively Unstable Regions in Supernovae
20.3.7 Remnants of Core Collapse
20.4 Supernova 1987A
20.4.1 The Neutrino Burst
20.4.2 The Progenitor was Blue!
20.4.3 Radioactive Decay and the Lightcurve
20.4.4 Evolution of the Supernova Remnant
20.4.5 Where is the Neutron Star?
20.5 Heavy Elements and the r-Process
Background and Further Reading
Problems
21 Gamma-Ray Bursts
21.1 The Sky in Gamma-Rays
21.2 Localization of Gamma-Ray Bursts
21.3 Generic Characteristics of Gamma-Ray Burst
21.4 The Importance of Ultrarelativistic Jets
21.4.1 Optical Depth for a Nonrelativistic Burst
21.4.2 Optical Depth for an Ultrarelativistic Burst
21.4.3 Confirmation of Large Lorentz Factors
21.5 Association of GRBs with Galaxies
21.6 Mechanisms for the Central Engine
21.7 Long-Period GRB and Supernovae
21.7.1 Types Ib and Ic Supernovae
21.7.2 Role of Metallicity
21.8 Collapsar Model of Long-Period Bursts
21.9 Neutron Star Mergers and Short-Period Bursts
21.10 Multimessenger Astronomy
Background and Further Reading
Problems
22 Gravitational Waves and Stellar Evolution
22.1 Gravitational Waves
22.2 Sample Gravitational Waveforms
22.3 The Gravitational Wave Event GW150914
22.3.1 Observed Waveforms
22.3.2 The Black Hole Merger
22.4 A New Probe of Massive-Star Evolution
22.4.1 Formation of Massive Black Hole Binaries
22.4.2 Gravitational Waves and Massive Binary Evolution
22.4.3 Formation of Supermassive Black Holes
22.5 Listening to Multiple Messengers
22.6 Gravitational Waves from Neutron Star Mergers
22.6.1 New Insights Associated with GW170817
22.6.2 The Kilonova Associated with GW170817
22.7 Gravitational Wave Sources and Detectors

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