Title:

Problems in relativistic cosmology

After a brief survey of the cosmological features of the observable universe the two main techniques used in theoretical cosmology are developed. These are the Kinematic technique as first used in Kinematic Relativity, based on the concept of a Kinematic equivalence, and the Riemannian technique as first used in General relativity based on the concept of a Riemannian spacetime map. Formulae for proper distance, red=shift, etc. are developed independently in each technique. Others like nebular count formulae, which are less readily amenable to the Kinematic technique, are discussed by the Riemannian technique only. The two techniques pre then correlated. It is found that any homogeneous and isotropic modeluniverse with given Kinematic properties can be described end discussed in terms of either technique and that a relation exists between the arbitrary elements in the two descriptions. It is shown how formulae associated with either technique can be translated into formulae associated with the other. Thus the geometric apparatus of the Riemannian technique end other useful formulae become available to the Kinematic technique. The correlation extends the scope of the Kinematic technique and at the same time throws light on certain aspects of the Riemannian technique. The redshift formulae developed earlier are now used to analyse the new HumasonMayallSandage data on redshifts. It is found that these rule out all but decelerating model=universes unless some further hypotheses are made. The particular hypothesis of varying absolute nebular luminosities is examined and the minimum rate required is found. The last chapter contains e complete analysis of visual horizons in cosmology. Two essentially different types of horizon are recognized end examples are given of models possessing either type, both types at once, or no horizon. In an appendix the tensor significance of the "relativistic" acceleration, as used e.g. in Page's equivalence, is investigated.
