The Solar Chromosphere and Corona: Quiet Sun

I. Introduction.- 1. Chromospheres and Coronas.- 2. Goals for Solar Physics.- 3. Chromosphere and Coronal Boundaries.- 4. Methods of Observation.- 5. The K- and F-Coronas.- 6. Comments on Discrete Geometrical Features.- 7. Depths of Line Formation.- II. Structural Features.- 1. Observational Methods.- 2. The Photospheric Structure.- 3. Chromospheric Network.- 4. Chromospheric Fine Structure on the Disk.- 5. Spicule Structure.- 6. Transition Region Structure.- 7. Non-Spherical Modeling.- 8. Chromospheric Active Region Structure.- 9. Observations of Coronal Structures.- 10. Fine Structure of Inner Corona.- 11. Coronal Streamers.- 12. Coronal Rays and Plumes.- 13. Coronal Disk Structures and Coronal Holes.- 14. Prominences.- 15. Solar Cycle Effects.- III. Macroscopic Motions.- 1. Measuring Systematic Motions.- 2. Photospheric Motions.- A. Wave Frequency.- B. Phase Relations.- C. Velocity Amplitude and Cell Size.- D. Discussion.- 3. Chromospheric Motions.- A. Spicules and Fibrils.- B. Cell Bright Points.- C. Chromospheric Oscillations.- D. Doppler Broadening of Chromospheric Lines.- 4. Small Scale Coronal Motions.- 5. Coronal Expansion: The Solar Wind.- 6. Prominence Motions.- 7. Impulsive Motions.- 8. Mass Balance and Energy Transport in Mass Flow.- IV. Magnetic Fields.- 1. Method of Observation.- 2. Energy Considerations.- 3. Polar Fields and UM Regions.- 4. Evolution of Large Scale Fields.- 5. Structure and Evolution of Small Scale Fields.- 6. Coronal Magnetic Fields.- V. Spectral Characteristics.- 1. Visual and Near Infrared Disk.- 2. Visual and Near Infrared Limb.- A. Chromospheric Eclipse Data.- B. Chromospheric Limb Outside of Eclipse.- C. Coronal Eclipse Data.- D. Coronal Limb Data Outside of Eclipse.- 3. Infrared, Radio and XUV Continuum Data.- A. Infrared and Radio Data.- B. XUV Data.- 4. XUV Emission Lines.- VI. Analytical Methods for Spectroscopic Data.- 1. Scattering Continuum.- A. Electron Scattering.- B. Rayleigh Scattering.- 2. Bound-Free Continua: Effectively Thin Case.- A. H-.- B. Balmer and Paschen Bound-Free Continua.- C. Helium Bound-Free Continua.- 3. Free-Free Continua.- 4. Total Line Intensities: Effectively Thin Case.- A. Two-Level Atom.- B. Three-Level Atom.- 5. Profiles of lines and Bound-Free Continua: Effectively Thick Case.- A. A Form of the Line Transfer Equation for Non-Coherent Scattering.- B. Solution of the Pseudo Line Transfer Equation.- C. The Influence of a Chromosphere.- D. Multilevel Effects.- E. Lines Formed by Coherent Scattering and Bound-Free Continua.- VII. Empirical Chromospheric and Coronal Models.- 1. Summary Models.- 2. Conditions at the Optical Limb.- 3. The Temperature Minimum Region.- A. Radiation Losses.- B. Empirical Determination of Tmin.- 4. The Low Chromosphere.- 5. The Middle Chromosphere.- A. General Comments.- B. Visual Continuum.- C. Lyman Continuum.- D. Spectral Lines on the Disk.- E. Helium lines.- 6. The High Chromosphere.- A. Mean Spherically Symmetric Model.- B. Spicule Models.- C. Spectral Line Intensities.- 7. The Chromosphere-Corona Transition Region.- 8. The Corona.- A. Density Models.- B. Ionization Temperature.- C. Line Width Temperatures.- D. Line Intensity Ratios.- E. Radio Temperatures.- F. Temperature Distribution.- VIII. Chromospheric Structure Inferred from Spectral Lines.- 1. Chromospheres and Coronas as Phenomena of Stellar Atmospheres.- 2. Influence of the Chromospheric Temperature Rise.- 3. Influence of the Chromospheric Increase in Doppler Width.- 4. Ca ii lines.- 5. Mg ii Lines.- 6. Neutral Metal Lines.- 7. Hydrogen Lines.- 8. C ii and O i Lines.- 9. Summary.- IX. Energy and Momentum Balance.- 1. Energy Balance.- 2. Radiation Loss Rates.- 3. Thermal Stability.- 4. Coronal Energy Loss by Thermal Conduction and Evaporation.- 5. Energy Balance Within the Transition Region.- 6. The Base of the Transition Region.- 7. The Effect of Motions.- 8. Energy Losses from the Chromosphere.- A. Upper Chromosphere.- B. Middle Chromosphere.- C. Low Chromosphere and Tmin Region.- 9. The Quiet Sun Solar Wind.- A. An Inconsistency of Hydrostatic Equilibrium.- B. Isothermal and Polytropic Expansion.- C. Expansion Combined with Thermal Conduction.- D. Two-Fluid Models.- E. Evaporative Models.- F. The Observational Solar Wind.- 10. Spicule Mechanisms.- A. Summary of Spicule Characteristics.- B. Summary of Theoretical Models.- C. Shock Wave Models.- D. Jets Driven by Gas Pressure.- E. Jets Driven by a Combination of Gas Pressure and Hydrodynamic Forces.- F. Jets Driven by Radiation Pressure.- G. Magnetically Driven Spicules.- X. Wave Generation and Heating.- 1. Wave Generation.- A. Expected Wave Modes.- B. Wave Equations.- C. Acoustic-Gravity Waves.- D. Magneto-Acoustic Waves.- E. Magneto-Acoustic-Gravity Waves.- 2. Interpretation of 5 Minute Oscillations.- A. Location of Waves in ki, ?1 Plane.- B. Models for 5 Minute Oscillations.- 3. Generation of Waves by the Convection Zone.- A. Convective Overshoot.- B. Overstability.- C. Convective Compression.- 4. Heating.- A. Chromospheric Models.- B. Transition Region and Coronal Models.- 5. Acoustic Production of Stellar Chromospheres and Coronas.