Physics of the Sun: A First Course

The Global Parameters of the Sun Orbital Motion of the Earth Astronomical Unit (AU) GM and the Mass of the Sun Power Output of the Sun: The Solar Luminosity Radius of the Sun: R Surface Gravity of the Sun Escape Speed from the Solar Surface Effective Temperature of the Sun Shape of the Sun Critical Frequency for Solar Oscillations Mean Density of the Sun Radiation Flow through the Solar Atmosphere Radiation Field in the Solar Atmosphere Empirical Properties of the Radiant Energy from the Sun RTE Optical Depth and the Concept of "the Photosphere" Special Solutions of the RTE Eddington-Barbier Relationship Is Limb Brightening Possible? Is S(tau) = a + b tau Realistic? The Gray Atmosphere How Does Temperature Vary as a Function of tau? Properties of the Eddington Relation Toward a Model of the Sun: Opacity Relationship between Optical Depth and Linear Absorption Coefficient Two Approaches to Opacity: Atomic and Astrophysical Atomic Physics: (i) Opacity due to Hydrogen Atoms Atomic Physics: (ii) Opacity due to Negative Hydrogen Ions Atomic Physics: (iii) Opacity due to Helium Atoms and Ions Astrophysics: The Rosseland Mean Opacity Power-Law Approximations to the Rosseland Mean Opacity Narrow Band Opacity: Absorption Lines in the Spectrum Toward a Model of the Sun: Ionization Statistical Weights of Free Electrons Saha Equation Application of the Saha Equation to Hydrogen in the Sun Application of the Saha Equation to Helium in the Sun Contours of Constant Ionization: The Two Limits Application of the Saha Equation to the Negative Hydrogen Ion Computing a Model of the Sun: The Photosphere Hydrostatic Equilibrium: The Scale Height Sharp Edge of the Sun's Disk Preparing to Compute a Model of the Solar Photosphere Computing a Model of the Photosphere: Step by Step The Outcome of the Calculation Overview of the Model of the Solar Photosphere Convection in the Sun: Empirical Properties Nonuniform Brightness Granule Shapes Upflow and Downflow Velocities Linear Sizes of Granules Circulation Time around a Granule Temperature Differences between Bright and Dark Gas Energy Flux Carried by Convection Onset of Convection in the Sun: The Critical Gradient gad Numerical Value of gad Alternative Expression for gad Computing a Model of the Sun: The Convection Zone Quantifying the Physics of Convection: Vertical Acceleration Velocities and Vertical Length Scales Mixing Length Theory (MLT) of Convection Temperature Excesses Associated with MLT Convection MLT Convective Flux in the Photosphere MLT Convective Flux below the Photosphere Adiabatic and Nonadiabatic Processes Computing a Model of the Convection Zone: Step by Step Overview of Our Model of the Convection Zone Radiative Transfer in the Deep Interior of the Sun Thermal Conductivity for Photons Flux of Radiant Energy at Radius r Base of the Convection Zone Temperature Gradient in Terms of Luminosity Temperature Gradient in Terms of Pressure Integrating the Temperature Equation Computing a Mechanical Model of the Sun: The Radiative Interior Computational Procedure: Step by Step Overview of Our Model of the Sun's Radiative Interior Photons in the Sun: How Long before They Escape? Global Property of the Solar Model Does the Material in the Sun Obey the Perfect Gas Law? Summary of Our Solar Model Polytropes Power-Law Behavior Polytropic Gas Spheres Lane-Emden Equation: Dimensional Form Lane-Emden Equation: Dimensionless Form Boundary Conditions for the Lane-Emden Equation Analytic Solutions of the Lane-Emden Equation Are Polytropes Relevant for "Real Stars"? Calculating a Polytropic Model: Step by Step Central Condensation of a Polytrope Energy Generation in the Sun pp-I Cycle of Nuclear Reactions Reaction Rates in the Sun Proton Collision Rates in the Sun Conditions Required for Nuclear Reactions in the Sun Rates of Thermonuclear Reactions: Two Contributing Factors Temperature Dependence of Thermonuclear Reaction Rates Rate of Reaction (c) in the pp-cycle Neutrinos from the Sun Generation and Propagation of Solar Neutrinos Fluxes of Solar Neutrinos at the Earth's Orbit Neutrinos from Reactions other than pp-I Detecting Solar Neutrinos on Earth Solution of the Solar Neutrino Problem Oscillations in the Sun: The Observations Variability in Time Only Variability in Space and Time Radial Order of a Mode Which p-Modes have the Largest Amplitudes? Trapped and Untrapped Modes Long-Period Oscillations in the Sun Oscillations in the Sun: Theory Small Oscillations: Deriving the Equations Conversion to Dimensionless Variables Overview of the Equations The Simplest Exercise: Solutions for the Polytrope n = 1 What about g-Modes? Asymptotic Behavior of the Oscillation Equations Depth of Penetration of p-Modes beneath the Surface of the Sun Why are Certain Modes Excited More than Others in the Sun? Using Helioseismology to Test a Solar Model The Chromosphere Definition of the Chromosphere Linear Thickness of the Chromosphere Observing the Chromosphere on the Solar Disk Appearance of the Chromosphere on the Disk Properties of Supergranules in the CaK Line Supergranules Observed in the Ha Line The Two Principal Components of the Chromosphere Temperature Increase into the Chromosphere: Empirical Results Temperature Increase into the Chromosphere: Mechanical Work Modeling the Chromosphere: The Input Energy Flux Modeling the Chromosphere: Depositing the Energy Modeling the Equilibrium Chromosphere: Radiating the Energy Away Magnetic Fields in the Sun Sunspots Chromospheric Emission Magnetic Fields: The Source of Solar Activity Measurements of Solar Magnetic Fields Empirical Properties of Solar Magnetic Fields Interactions between Magnetic Fields and Ionized Gas Understanding Magnetic Structures in the Sun Amplification of Strong Solar Magnetic Fields Why Does the Sun Have a Magnetic Cycle with P " 10 Years? Releases of Magnetic Energy The Corona Electron Densities Spatial Structure in the White Light Corona Electron Temperatures Temperature of Line Formation Pressure Scale Heights in the Corona Ion Temperatures X-Ray Line Strengths: The Emission Measure Densities and Temperatures: Quiet Sun versus Active Regions Gas Pressures in the Corona Spatial Structure in the X-Ray Corona Magnetic Structures: Loops in Active Regions Magnetic Structures: Coronal Holes Magnetic Structures: The Quiet Sun Why Are Quiet Coronal Temperatures of Order 1-2MK? Abrupt Transition from Chromosphere to Corona Rate of Mechanical Energy Deposition in the Corona What Heats the Corona? Solar Flares The Solar Wind Global Breakdown of Hydrostatic Equilibrium in the Corona Localized Applicability of HSE Solar Wind Expansion: Steady State Flow Observational Evidence for Solar Wind Acceleration Energy Equation Asymptotic Speed of the Solar Wind Rate of Mass Outflow from the Sun Coronal Mass Ejections How Far Does the Sun's Influence Extend in Space? Appendix Index Exercises and References appear at the end of most chapters.