![Masters Theses](../../assets/md5images/ebc0648ded2cd429f55e0a2fe4407546.gif)
Masters Theses
Date of Award
5-1998
Degree Type
Thesis
Degree Name
Master of Science
Major
Physics
Major Professor
Horace Crater
Committee Members
Trevor Moulden, Christian Parigger
Abstract
The standard Friedmann-Robertson-Walker ( FRW ) cosmological model is modified by including a time dependent eccentricity term ε(t) in the metric tensor that describes the oblateness for an expanding hyperellipsoid. The oblateness dissipates when cosmic time is much greater than a characteristic time tchar, on the order of a fraction of the Hubble time, consequently the geometry of space-time reduces to that of a perfect hypersphere.
The metric tensor gμv retains a diagonal matrix form, but the inclusion of the eccentricity term will generate off-diagonal terms G01, and G10 in the Einstein tensor gμv If the stress-energy tensor is described by an imperfect relativistic fluid, then a time dependent thermal gradient will appear as a non-diagonal term. This term is a function of the eccentricity ε(t), and may account for thermal equilibrium during the initial stages of development for the universe. A numerical solution for the cosmic radius R(t) is presented.
Recommended Citation
Stein, Charles Shane, "A metric tensor in cosmology. " Master's Thesis, University of Tennessee, 1998.
https://trace.tennessee.edu/utk_gradthes/10372