Show full item record Abstract The focus of this thesis is on numerical modeling of fluid-structure interaction FSI problems with application to hemodynamics.
Interaction of magnetic field and flow in the outer shells of giant planets Citation Liu, Junjun Interaction of magnetic field and flow in the outer shells of giant planets. The atmospheres of Jupiter and Saturn exhibit strong and stable zonal winds.
Busse suggested that they might be the surface expression of deep flows on cylinders. However, the deep flow hypothesis experiences difficulty when account is taken of the electrical conductivity of molecular hydrogen as measured in shockwave experiments.
The deep zonal flow of an electrically conducting fluid would produce a toroidal magnetic field, an associated poloidal electrical current, and Ohmic dissipation.
In steady state, the total Ohmic dissipation cannot exceed the planet's net luminosity. If we assume that the observed zonal flow penetrates along cylinders until it is truncated to near zero at some spherical radius, the upper bound on Ohmic dissipation constrains this radius to be no smaller than 0.
The truncation of the cylindrical flow in the convective envelope requires an appropriate force to break the Taylor-Proudman constraint.
We have been unable to identify any plausible candidate. Thus we conclude that deep-seated cylindrical flows do not exist. A fluid shell with sufficient electrical conductivity and azimuthal velocity shear outside of the dynamo generation region can attenuate the non-axisymmetric component of the magnetic field.
However, the interaction of the axisymmetric component of the magnetic field and the zonal flow is able to reduce the magnitude of zonal flow. The dimensionless number characterizing this reduction is the Chandrasekhar number. The smaller Saturnian field may allow a larger velocity shear and a greater attenuation of the non-axisymmetric field, thereby providing a possible explanation for the nearly axisymmetric field.
Combining the study for the attenuation effect produced by the semi-conducting layer and the observation of the magnetic field by Galileo and Voyager, we find the possible outer boundary of the dynamo generation zone is at 0.
The magnetic fields generated in the outer shell are dictated by a length scale comparable to the scale height of electrical conductivity, which is much smaller than the radius of the planet.Thesis and Graduation ; CNSU Elections ; Computational modelling of fluid-structure interaction.
Computational modelling of fluid-structure interaction. 1 Research Collaborator position. Fields: Computational fluid dynamics, Finite element method, Shells and laminate structures, Photovoltaic modules. Advances in Computational Methods for Fluid-Structure-Interaction Problems Thesis directed by Professor Thomas L.
Geers Part 1: Response of Empty and Fluid-Filled, Submerged Spherical Shells to . A thesis presented to Ryerson University in partial fulfillment of the requirements for the degree of The description of a fluid structure interaction between a fluid and a rod is as follows : 1.
The moving fluid creates a load on the rod 2. The rod deforms under the load. MASTER’S THESIS IN SOLID AND STRUCTURAL MECHANICS AND FLUID DYNAMICS Fluid Structure Interaction on Wind Turbine Blades JONAS NORLIN CHRISTOFFER JARPNER. Fluid-structure interaction between an incompressible, viscous 3D fluid and an elastic shell with nonlinear Koiter membrane energy Boris Muha Sun cica Cani c y Abstract.
Review of studies on geometrically nonlinear vibrations and dynamics of circular cylindrical shells and panels, with and without fluid-structure interaction.