Galaxy Formation in the Early Universe

Abstract

A ‘ spinning-core ’ theory of the origin and formation of galaxies is proposed and discussed. The initial cosmological state consists of metric fluctuations of which the energy and spin fluctuations are the initial conditions of galaxy formation. These initial conditions imply that relatively dense rotating cores develop in the radiation era of the fireball. The mass, and the energy and spin fluctuation parameters β E and β S determine the main properties of the cores. Some basic problems in the study of galaxy formation are discussed and it is argued that current ideas are apparently inadequate to solve these problems. It is then shown semi-quantitatively that the ‘ spinning-core ’ theory is capable of explaining the morphology and structural complexity of galaxies. In particular, when $${\beta\,S}\,\lt\,{\beta\,E}$$ the cores evolve into ellipticals, and when $${\beta\,S}\,\gt\,{\beta\,E}$$ they evolve into spirals. Cores of $${\beta\,S}\,\lt\,{\beta\,E}^{2}$$ remain as massive unborn galaxies and may constitute the major fraction of the mass of the Universe; cores of $${\beta\,S}\,\sim\,{\beta\,E}^{2}$$ , however, lie dormant for long periods of time and then flare up as little-bangs and are therefore an attractive possible explanation of eruptive galactic nuclei and quasi-stellar sources.