A. D. Linde's Particle Physics and Inflationary Cosmology PDF

By A. D. Linde

ISBN-10: 3718604906

ISBN-13: 9783718604906

This quantity is an entire and systematic monograph on inflationary cosmology and cosmological section transitions. Dr. Linde, a first-rate developer of those theories, deals a radical research of contemporary cosmology and its relation to hassle-free particle physics, together with a wide introductory part containing an entire dialogue of inflationary cosmology for these now not but acquainted with the speculation.

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Additional resources for Particle Physics and Inflationary Cosmology

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Meanwhile, the results of the preceding section make it clear that the observable part of the universe is most likely just a minuscule part of the universe as a whole, and it is an impermissible extrapolation to draw any conclusions about the homogeneity of the latter based on observations of such a tiny component. On the contrary, an investigation of the global geometry of the inflationary universe shows that the universe, which is locally Friedmann, should be completely inhomogeneous on the largest scales, and its global geometry and dynamical behavior as a whole have nothing in common with the geometry and dynamics of a Friedmann universe [57, 78, 133, 134].

8), that the vacuum energy density does not change as the universe expands (a “void” remains a “void”, even if it has weight). 3) for k = 0 (a flat universe), and 8π 8πρ . More generally, during Gρ = 3 3 M2P expansion the magnitude of H in the inflationary universe scenario changes, but very slowly, ˙ ≪ H2 . 4) for k = −1 (an open universe). 5) or of a quasi-de Sitter stage in its expansion; just this regime of quasiexponential expansion is known as inflation. Inflation comes to an end when H begins to decrease rapidly.

This would of course have catastrophic consequences, as the mass of each monopole is perhaps 1016 times that of the proton, giving an energy density in the universe about 15 orders of magnitude higher than the critical density ρc ∼ 1029 g/cm3 . At that density, the universe would have collapsed long ago. The primordial monopole problem is one of the sharpest encountered thus far by elementary particle theory and cosmology, since it relates to practically all unified theories of weak, strong, and electromagnetic interactions.

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Particle Physics and Inflationary Cosmology by A. D. Linde


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