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• W590902564 abstract "The Global Parameters of Sun Orbital Motion of Earth Astronomical Unit (AU) GM and Mass of Sun Power Output of Sun: The Solar Luminosity Radius of Sun: R Surface Gravity of Sun Escape Speed from Solar Surface Effective Temperature of Sun Shape of Sun Critical Frequency for Solar Oscillations Mean Density of Sun Radiation Flow through Solar Atmosphere Radiation Field in Solar Atmosphere Empirical Properties of Radiant Energy from Sun RTE Optical Depth and Concept of the Special Solutions of 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 Eddington Relation Toward a Model of 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 Rosseland Mean Opacity Narrow Band Opacity: Absorption Lines in Spectrum Toward a Model of Sun: Ionization Statistical Weights of Free Electrons Saha Equation Application of Saha Equation to Hydrogen in Sun Application of Saha Equation to Helium in Sun Contours of Constant Ionization: The Two Limits Application of Saha Equation to Negative Hydrogen Ion Computing a Model of Sun: The Photosphere Hydrostatic Equilibrium: The Scale Height Sharp Edge of Sun's Disk Preparing to Compute a Model of Solar Photosphere Computing a Model of Photosphere: Step by Step The Outcome of Calculation Overview of Model of Solar Photosphere Convection in 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 Sun: The Critical Gradient gad Numerical Value of gad Alternative Expression for gad Computing a Model of Sun: The Convection Zone Quantifying 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 Photosphere MLT Convective Flux below Photosphere Adiabatic and Nonadiabatic Processes Computing a Model of Convection Zone: Step by Step Overview of Our Model of Convection Zone Radiative Transfer in Deep Interior of Sun Thermal Conductivity for Photons Flux of Radiant Energy at Radius r Base of Convection Zone Temperature Gradient in Terms of Luminosity Temperature Gradient in Terms of Pressure Integrating Temperature Equation Computing a Mechanical Model of Sun: The Radiative Interior Computational Procedure: Step by Step Overview of Our Model of Sun's Radiative Interior Photons in Sun: How Long before They Escape? Global Property of Solar Model Does Material in Sun Obey 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 Lane-Emden Equation Analytic Solutions of Lane-Emden Equation Are Polytropes Relevant for Real Stars? Calculating a Polytropic Model: Step by Step Central Condensation of a Polytrope Energy Generation in Sun pp-I Cycle of Nuclear Reactions Reaction Rates in Sun Proton Collision Rates in Sun Conditions Required for Nuclear Reactions in Sun Rates of Thermonuclear Reactions: Two Contributing Factors Temperature Dependence of Thermonuclear Reaction Rates Rate of Reaction (c) in pp-cycle Neutrinos from Sun Generation and Propagation of Solar Neutrinos Fluxes of Solar Neutrinos at Earth's Orbit Neutrinos from Reactions other than pp-I Detecting Solar Neutrinos on Earth Solution of Solar Neutrino Problem Oscillations in Sun: The Observations Variability in Time Only Variability in Space and Time Radial Order of a Mode Which p-Modes have Largest Amplitudes? Trapped and Untrapped Modes Long-Period Oscillations in Sun Oscillations in Sun: Theory Small Oscillations: Deriving Equations Conversion to Dimensionless Variables Overview of Equations The Simplest Exercise: Solutions for Polytrope n = 1 What about g-Modes? Asymptotic Behavior of Oscillation Equations Depth of Penetration of p-Modes beneath Surface of Sun Why are Certain Modes Excited More than Others in Sun? Using Helioseismology to Test a Solar Model The Chromosphere Definition of Chromosphere Linear Thickness of Chromosphere Observing Chromosphere on Solar Disk Appearance of Chromosphere on Disk Properties of Supergranules in CaK Line Supergranules Observed in Ha Line The Two Principal Components of Chromosphere Temperature Increase into Chromosphere: Empirical Results Temperature Increase into Chromosphere: Mechanical Work Modeling Chromosphere: The Input Energy Flux Modeling Chromosphere: Depositing Energy Modeling Equilibrium Chromosphere: Radiating Energy Away Magnetic Fields in 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 Sun Amplification of Strong Solar Magnetic Fields Why Does Sun Have a Magnetic Cycle with P 10 Years? Releases of Magnetic Energy The Corona Electron Densities Spatial Structure in White Light Corona Electron Temperatures Temperature of Line Formation Pressure Scale Heights in Corona Ion Temperatures X-Ray Line Strengths: The Emission Measure Densities and Temperatures: Quiet Sun versus Active Regions Gas Pressures in Corona Spatial Structure in 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 Corona What Heats Corona? Solar Flares The Solar Wind Global Breakdown of Hydrostatic Equilibrium in Corona Localized Applicability of HSE Solar Wind Expansion: Steady State Flow Observational Evidence for Solar Wind Acceleration Energy Equation Asymptotic Speed of Solar Wind Rate of Mass Outflow from Sun Coronal Mass Ejections How Far Does Sun's Influence Extend in Space? Appendix Index Exercises and References appear at end of most chapters." @default.
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• W590902564 date "2009-08-26" @default.
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• W590902564 title "Physics of the Sun: A First Course" @default.
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