Download An introduction to mathematical cosmology by J. N. Islam PDF

By J. N. Islam

ISBN-10: 0511018495

ISBN-13: 9780511018497

This ebook presents a concise creation to the mathematical facets of the foundation, constitution and evolution of the universe. The ebook starts off with a quick review of observational and theoretical cosmology, in addition to a quick creation of basic relativity. It then is going directly to speak about Friedmann versions, the Hubble consistent and deceleration parameter, singularities, the early universe, inflation, quantum cosmology and the far away way forward for the universe. This re-creation includes a rigorous derivation of the Robertson-Walker metric. It additionally discusses the bounds to the parameter house via quite a few theoretical and observational constraints, and offers a brand new inflationary resolution for a 6th measure capability. This publication is acceptable as a textbook for complex undergraduates and starting graduate scholars. it's going to even be of curiosity to cosmologists, astrophysicists, utilized mathematicians and mathematical physicists.

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2) satisfies the geodesic equation d2x␮ dx␭ dx␯ ϭ0. 4) is satisfied if ⌫␮00 ϭ0. In fact ⌫␮00 ϭ 12 ␮␯(2 ␯0,0 Ϫ 00,␯). 2) are indeed geodesics. 1) does not incorporate the property that space is homogeneous and isotropic. This form of the metric can be used, with the help of a special coordinate system obtained by singling out a particular typical galaxy, to derive some general properties of the universe without the assumptions of homogeneity and isotropy (see, for example, Raychaudhuri (1955)). 1) when space is homogeneous and isotropic.

This definition cannot be taken over directly to general relativity. 4). One therefore has to find some coordinate independent and covariant manner of defining space-time symmetries such as axial symmetry and stationarity. This is done with the help of Killing vectors, which we will now consider. In some cases there is a less rigorous but simpler way of deriving the metric which we will also consider. In the following we will sometimes write x, y, xЈ for x␮, y␮, xЈ␮ respectively. A metric ␮␯(x) is form-invariant under a transformation from x␮ to xЈ␮ if ␮␯ Ј (xЈ) is the same function of xЈ␮ as ␮␯(x) is of x␮.

109) we get u␯u␯;␴ ϭ0. 111) in electromagnetic theory, so we can define a scalar field ␳ and the corresponding vector field ␳u␮ which determine the density and flow of matter. 73) and following discussion) that the ordinary density of matter is not a component of a four-vector, but that of a fourvector density, which is obtained by multiplying the four-vector by 1 ϭ(Ϫ )2. Thus the density here is given by ␳u0 and the flow or the current by ␳ui (iϭ1,2,3). 72)) (␳u␮);␮ ϭ0. 112) The matter under consideration has energy density (␳u0)u0 and energy flux (␳u0)ui .

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