دانلود کتاب Exoplanetary Atmospheres: Theoretical Concepts and Foundations

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Contents\nForeword\nPreface\n1. \rObservations of Exoplanetary Atmospheres: A Theorist’s Review of Techniques in Astronomy\n 1.1 The birth of exoplanetary science\n 1.2 Transits and occultations\n 1.3 Radial velocity measurements\n 1.4 Direct imaging\n 1.5 Gravitational microlensing\n 1.6 Future missions and telescopes\n2.\r Introduction to Radiative Transfer\n 2.1 The optical depth: The most fundamental quantity in radiative transfer\n 2.2 Basic quantities in radiative transfer\n 2.3 The radiative transfer equation\n 2.4 Simple solutions of the radiative transfer equation\n 2.5 A practical checklist for radiative transfer calculations\n 2.6 Clouds\n 2.7 Atmospheric retrieval\n 2.8 Problem sets\n3.\r The Two-Stream Approximation of Radiative Transfer\n 3.1 What is the two-stream approximation?\n 3.2 The radiative transfer equation and its moments\n 3.3 Two-stream solutions with isotropic scattering\n 3.4 The scattering phase function\n 3.5 Two-stream solutions with non-isotropic scattering\n 3.6 Different closures of the two-stream solutions\n 3.7 The diffusion approximation for radiative transfer\n 3.8 Problem sets\n4.\r Temperature-Pressure Profiles\n 4.1 A myriad of atmospheric effects: Greenhouse warming and antigreenhouse cooling\n 4.2 The dual-band or double-gray approximation\n 4.3 The radiative transfer equation and the scattering parameter\n 4.4 Treatment of shortwave radiation\n 4.5 Treatment of longwave radiation\n 4.6 Assembling the pieces: Deriving the general solution\n 4.7 Exploration of different atmospheric effects\n 4.8 Milne’s solution and the convective adiabat\n 4.9 Problem sets\n5.\r Atmospheric Opacities: How to Use a Line List\n 5.1 From spectroscopic line lists to synthetic spectra\n 5.2 The Voigt profile\n 5.3 The quantum physics of spectral lines\n 5.4 The million- to billion-line radiative transfer challenge\n 5.5 Different types of mean opacities\n 5.6 Problem sets\n6. Introduction to Atmospheric Chemistry\n 6.1 Why is atmospheric chemistry important?\n 6.2 Basic quantities: Gibbs free energy, equilibrium constant, rate coefficients\n 6.3 Chemical kinetics: Treating chemistry as a set of mass conservation equations\n 6.4 Self-consistent atmospheric chemistry, radiation and dynamics: A formidable computational challenge\n 6.5 Problem sets\n7.\r A Hierarchy of Atmospheric Chemistries\n 7.1 A hierarchy of models for understanding atmospheric chemistry\n 7.2 Equilibrium chemistry with only hydrogen\n 7.3 Equilibrium C-H-O chemistry: Forming methane, water, carbon monoxide and acetylene\n 7.4 Equilibrium C-H-O chemistry: Adding carbon dioxide\n 7.5 Equilibrium C-H-O chemistry: Adding ethylene\n 7.6 Problem sets\n8.\r Introduction to Fluid Dynamics\n 8.1 Why is the study of fluids relevant to exoplanetary atmospheres?\n 8.2 What exactly is a fluid?\n 8.3 The governing equations of fluid dynamics\n 8.4 Potential temperature and potential vorticity\n 8.5 Dimensionless fluid numbers\n 8.6 Problem sets\n9.\r Deriving the Governing Equations of Fluid Dynamics\n 9.1 Preamble\n 9.2 The mass continuity equation (mass conservation)\n 9.3 The Navier-Stokes equation (momentum conservation)\n 9.4 The thermodynamic equation (energy conservation)\n 9.5 The conservation of potential vorticity\n 9.6 Various approximate forms of the governing equations of fluid dynamics\n 9.7 Magnetohydrodynamics\n 9.8 Problem sets\n10.\r The Shallow Water System: A Fluid Dynamics Lab on Paper\n 10.1 A versatile fluid dynamics laboratory on paper\n 10.2 Deriving the shallow water equations\n 10.3 Gravity as the restoring force: The generation of gravity waves\n 10.4 Friction in an atmosphere: Molecular viscosity and Rayleigh drag\n 10.5 Forcing the atmosphere: Stellar irradiation\n 10.6 Like plucking a string: Alfvén waves\n 10.7 Rotation: The generation of Poincaré and Rossby waves\n 10.8 General coupling of physical effects\n 10.9 Shallow atmospheres as quantum harmonic oscillators\n 10.10 Shallow water systems and exoplanetary atmospheres\n 10.11 Problem sets\n11.\r The de Laval Nozzle and Shocks\n 11.1 What is the de Laval nozzle?\n 11.2 What are shocks?\n 11.3 What does the de Laval nozzle teach us about shocks?\n 11.4 Applications to, and consequences for, exoplanetary atmospheres\n 11.5 Problem sets\n12.\r Convection, Turbulence and Fluid Instabilities\n 12.1 Fluid motion induced by physically unstable configurations\n 12.2 Hot air rises and cold air sinks: Schwarzschild’s criterion for convective stability\n 12.3 A simplified “theory” of convection: Mixing length theory\n 12.4 Implementing convection in numerical calculations: Convective adjustment schemes\n 12.5 A simple “theory” of turbulence: The scaling laws of Kolmogorov\n 12.6 Water over oil: The Rayleigh-Taylor instability\n 12.7 Shearing fluids: The Kelvin-Helmholtz instability\n 12.8 Weather at mid-latitudes: The baroclinic instability\n 12.9 Problem sets\n13.\r Atmospheric Escape\n 13.1 The Knudsen number and Jeans parameter\n 13.2 Jeans escape\n 13.3 The classical Parker wind solution\n 13.4 Non-isothermal Parker winds: Using the nozzle solutions\n 13.5 Detailed processes: Photo-ionization, radiative cooling and nonthermal mechanisms\n 13.6 Problem sets\n14.\r Outstanding Problems of Exoplanetary Atmospheres\nAppendix A: Summary of Standard Notation\nAppendix B: Essential Formulae of Vector Calculus\nAppendix C: Essential Formulae of Thermodynamics\nAppendix D: Gibbs Free Energies of Various Molecules and Re-actions\nAppendix E: Python Scripts for Generating Figures\nBibliography\nIndex