Cosmic inflationInflation is the idea—first proposed by Alan Guth (1981)—that the nascent universe passed through a phase of exponential expansion (the inflationary epoch) that was driven by a negative vacuum energy density (positive vacuum pressure). This expansion can be modelled by a non-zero cosmological constant. As a direct consequence of this expansion, all of the observable universe is posited to have originated in a small, initially causally-connected region. Quantum fluctuations in this microscopic region, magnified to cosmic size, then became the seeds for the growth of structure in the universe (see Galaxy Formation and Evolution). Inflation resolves several problems in the Big Bang cosmology that were pointed out in the 1970s. Among these are the observed flatness of the universe (the flatness problem), its extraordinary homogeneity on large (non-causally-connected) scales (the horizon problem), and its lack of any observed topological defects (e.g., the monopole problem), predicted by many Grand Unified Theories. Predictions of the standard model of inflation include geometrical flatness of the universe to high precision and near scale invariance of the fluctuations in the cosmic microwave background. There are also consequences for high-energy particle physics near or at the GUT scale. During the 1980s, there were many attempts to relate the field that generates the vacuum energy to specific fields that were predicted by Grand Unified Theories or to use observations of the universe to constrain those theories. These efforts proved fruitless and the exact nature of the particle or field that generates the vacuum energy density for inflation (the "inflaton") remains a mystery. One major theoretical issue involving inflation is that it is unclear how one gets inflation to stop once it has started. In addition, inflation implies rapid cooling of the universe and therefore there must be a period of reheating after the end of the period of inflation. From the framework of inflation, one can predict the power spectrum of the universe (which is essentially the amount of lumpiness) and compare them with observations of the anisotropy of the cosmic background radiation and the distribution of galaxies as seen by galaxy surveys. One prediction is that there should be ripples in the power spectrum which are known as acoustic peaks which can be matched to the parameters of the universe. These have been observed by WMAP, and are considered to be evidence that the inflationary scenario is correct. One popular idea that has been suggested in the context of string theory and quantum gravity is that the universe actually contains many more dimensions of space than the three we experience in daily life, but that the universe only experienced inflation along the three normal dimensions of space, leaving the other dimensions to be microscopic. As of 2004, it is also unclear what relationship if any the period of cosmic inflation has to do with observations of an accelerating universe. The name of the theory was a semi-humorous reference to the economic inflation in the United States in the late 1970s. See also: Cosmology References
ca:Univers inflacionari it:Inflazione (cosmologia) ja:インフレーション理論 pl:Inflacja kosmologiczna sv:Inflation (kosmologi) Categories: Cosmology |
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