Introduction to Modeling Convection in Planets and Stars
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A01=Gary A. Glatzmaier
Advection
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Amplitude
Angular resolution
Approximation
Author_Gary A. Glatzmaier
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Boundary layer
Boundary value problem
Boussinesq approximation (water waves)
Buoyancy
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Category=PGC
Category=PHVB
Clockwise
Coefficient
Colatitude
Convection
Convection zone
Convective heat transfer
COP=United States
Coriolis force
Courant-Friedrichs-Lewy condition
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Diffusivity
Dispersion relation
Energy density
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Equation
Equation of state
Finite difference
Fluid parcel
Fourier series
Galerkin method
Gaussian quadrature
Giant planet
Gravitational acceleration
Heat capacity
Heat flux
Heat transfer
Hydrostatic equilibrium
Induction equation
Instability
Internal wave
Ionization
Kinetic energy
Language_English
Legendre function
Length scale
Linear equation
Linear stability
Magnetic diffusivity
Magnetic energy
Magnetic field
Mass flux
Numerical analysis
Numerical methods for ordinary differential equations
Order of magnitude
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Perfect gas
Phase velocity
Prandtl number
Pressure gradient
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Quantity
Rayleigh number
Reynolds number
Scale height
softlaunch
Spectral method
Stream function
Subroutine
Temperature
Temperature gradient
Temporal resolution
Thermal diffusivity
Time derivative
Vertical direction
Viscosity
Vorticity
Vorticity equation
Wavelength
Wavenumber
Product details
- ISBN 9780691141732
- Weight: 567g
- Dimensions: 152 x 235mm
- Publication Date: 24 Nov 2013
- Publisher: Princeton University Press
- Publication City/Country: US
- Product Form: Paperback
- Language: English
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This book provides readers with the skills they need to write computer codes that simulate convection, internal gravity waves, and magnetic field generation in the interiors and atmospheres of rotating planets and stars. Using a teaching method perfected in the classroom, Gary Glatzmaier begins by offering a step-by-step guide on how to design codes for simulating nonlinear time-dependent thermal convection in a two-dimensional box using Fourier expansions in the horizontal direction and finite differences in the vertical direction. He then describes how to implement more efficient and accurate numerical methods and more realistic geometries in two and three dimensions. In the third part of the book, Glatzmaier demonstrates how to incorporate more sophisticated physics, including the effects of magnetic field, density stratification, and rotation. Featuring numerous exercises throughout, this is an ideal textbook for students and an essential resource for researchers.
* Describes how to create codes that simulate the internal dynamics of planets and stars * Builds on basic concepts and simple methods * Shows how to improve the efficiency and accuracy of the numerical methods * Describes more relevant geometries and boundary conditions * Demonstrates how to incorporate more sophisticated physics
Gary A. Glatzmaier is professor of earth and planetary sciences at the University of California, Santa Cruz. He is a fellow of the American Academy of Arts and Sciences and a member of the National Academy of Sciences.
