The science of the origin, structure, and evolution of the Universe including the origin of galaxies, the chemical elements, and matter.
Fr.: cosmologie fractale
The postulate that the concentrations of matter in the Universe follow a → fractal structure over a wide range of scales.
keyhân-šenâsi-ye zamin-markazi (#)
Fr.: cosmologie géocentrique
A model of the Universe in which the Earth is centrally located and the Sun, planets, and stars revolve around the Earth.
keyhânšenâsi-ye hurmarkazi (#)
Fr.: cosmologie héliocentrique
A model of the Universe in which the Sun was centrally located.
Fr.: cosmologie hiérarchique
A cosmology characterized by clustering of galaxy clusters in increasingly larger systems.
Fr.: cosmologie newtonienne
The use of → Newtonian mechanics to derive homogeneous and isotropic solutions of → Einstein's field equations, which represent models of expanding Universe. The Newtonian cosmology deviates from the prediction of → general relativity in the general case of anisotropic and inhomogeneous models.
Fr.: cosmologie observationnelle
The application of observational data to the study of the Universe as a whole.
Fr.: cosmologie plasma
An alternative cosmology, initially conceived by Hannes Alfvén in the 1960s, that attempts to explain the development of the visible Universe through the interaction of electromagnetic forces on astrophysical plasma. Like the steady state model, plasma cosmology hypothesizes an evolving Universe without beginning or end.
Fr.: cosmologie standard
The conventional → Big Bang model, which is based on two assumptions: the → cosmological principle of homogeneity and isotropy leading to the → Robertson-Walker metric, and → Einstein's field equations of general relativity along with familiar properties of matter. This model is a remarkably successful operating hypothesis describing the evolution of the Universe from 1/100 second after the initial event through to the present day. It provides explanations for several basic problems such as: → Hubble's law of recession of galaxies, interpreted in terms of the expansion of the Universe; the abundances of the → light elements, in excellent agreement with the predictions of → primordial nucleosynthesis; and the thermal spectrum and angular isotropy of the → cosmic microwave background (CMB) radiation, as expected from a hot, dense early phase of expansion. For a non-standard model, see → ekpyrotic Universe.