Download the full-sized PDF of Simulations of Rotating Anelastic Convection: Entropy Boundary ConditionsDownload the full-sized PDF



Permanent link (DOI):


Export to: EndNote  |  Zotero  |  Mendeley


This file is in the following communities:

Graduate Studies and Research, Faculty of


This file is in the following collections:

Theses and Dissertations

Simulations of Rotating Anelastic Convection: Entropy Boundary Conditions Open Access


Other title
Type of item
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 of Physics
Date accepted
Graduation date
2017-06:Spring 2017
Master of Science
Degree level
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.
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.
Citation for previous publication

File Details

Date Uploaded
Date Modified
Audit Status
Audits have not yet been run on this file.
File format: pdf (Portable Document Format)
Mime type: application/pdf
File size: 18681121
Last modified: 2017:06:13 12:10:59-06:00
Filename: Cuff_Keith_O_201611_MSc.pdf
Original checksum: 216332ad81149e6b72fd25697ad38444
Well formed: false
Valid: false
Status message: Unexpected error in findFonts java.lang.ClassCastException: edu.harvard.hul.ois.jhove.module.pdf.PdfSimpleObject cannot be cast to edu.harvard.hul.ois.jhove.module.pdf.PdfDictionary offset=2744
Page count: 104
Activity of users you follow
User Activity Date