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Permanent link (DOI): https://doi.org/10.7939/R3CF9JK0D

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Simulations of Rotating Anelastic Convection: Entropy Boundary Conditions Open Access

Descriptions

Other title
Subject/Keyword
convection
anelastic
entropy
Type of item
Thesis
Degree grantor
University of Alberta
Author or creator
Cuff, Keith O
Supervisor and department
Heimpel, Moritz (Physics)
Examining committee member and department
Schmitt, Doug (Physics)
Flynn, Morris (Mechanical Engineering)
Sutherland, Bruce (Physics)
Department
Department of Physics
Specialization
Geophysics
Date accepted
2016-11-22T08:07:31Z
Graduation date
2017-06:Spring 2017
Degree
Master of Science
Degree level
Master's
Abstract
In this dissertation we focus on numerical models of rotating anelastic convection, in particular the entropy boundary condition, with application to the giant planets. The first chapter details atmospheric features of giant planets and the numerical formulation of anelastic convection. The second chapter details entropy gradient boundary conditions compared to constant entropy boundary conditions used in previous studies. The third chapter considers a Gaussian perturbation on the lower boundary condition to examine surface effects of a plume from the deep interior. The fourth chapter considers high resolution simulations that are closer to a planetary parameter space. Most previous works on models of anelastic convection use a constant entropy difference boundary condition. For a strongly stratified system this requires a large entropy gradient near the surface to maintain the difference. This makes for strong convection at the outer boundary that disrupts coherent vortices. We use constant entropy gradient boundary conditions with entropy sinks so that the convection is strongest at the inner boundary and grades into neutral buoyancy at the outer boundary. A thermal plume from the deep interior is modelled using a Gaussian perturbation on the lower boundary. The parametrization of the plume is examined considering its amplitude, width, the latitudinal offset, and the background convective state. The flow produced at the surface typically includes a constant cyclonic vortex at the pole and short lived anticyclones at a lower latitude. Lowering the Ekman number allows for models that are less viscous and more representative of planets. These models have relaxation oscilations that are relatively quiet at the minimum and produce strong storms at the peak. We use these models to study the quasiperiodic Great White Spot storms that are observed on Saturn with a periodicity of about 1 Saturnian year.
Language
English
DOI
doi:10.7939/R3CF9JK0D
Rights
This thesis is made available by the University of Alberta Libraries with permission of the copyright owner solely for the purpose of private, scholarly or scientific research. This thesis, or any portion thereof, may not otherwise be copied or reproduced without the written consent of the copyright owner, except to the extent permitted by Canadian copyright law.
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