Black Holes, Cosmology and Extra Dimensions by Kirill A Bronnikov PDF

By Kirill A Bronnikov

ISBN-10: 9814374202

ISBN-13: 9789814374200

Assuming foundational wisdom of specified and basic relativity, this booklet courses the reader on concerns surrounding black holes, wormholes, cosmology, and additional dimensions. Its first half is dedicated to neighborhood powerful box configurations (black holes and wormholes) more often than not relativity and the main correct of different theories: scalar-tensor, f(R) and multidimensional theories. the second one half is on cosmology, together with inflation and a unified description of the total evolution of the universe. The 3rd half matters multidimensional theories of gravity and incorporates a variety of unique effects got through the authors. Expository paintings is carried out for a mechanism of symmetries and primary constants formation, whereas the unique method of nonlinear multidimensional gravity that's capable of build a different standpoint describing various phenomena is highlighted.

a lot of the content material is new in ebook guides, since it was once formerly came across in basic terms in magazine guides, e.g. relating to ordinary black holes, numerous scalar box ideas, wormholes and their balance, and multidimensional gravity.

Readership: scholars and pros in astrophysics/cosmology.

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Additional resources for Black Holes, Cosmology and Extra Dimensions

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The metric coefficient g00 is always nonzero in coordinates belonging to a certain RF. A very important example is the 3D chronometric metric tensor hik : according to the above, its contravariant components coincide (up to the sign) with their 4D counterparts: hik = −g ik . 30) 38 Black Holes, Cosmology and Extra Dimensions It can be shown [297, 437] that the covariant components of the chronometric spatial metric tensor and its determinant are expressed in terms of 4D quantities as follows: gi0 gk0 g hik = −gik + , h = det(hik ) = − .

The summed force applied to a body at rest in a certain IRF is equal to zero, or, in other words, such a body moves by inertia, uniformly and straightly with respect to any other IRF. 1) where c is a universal constant coinciding with the propagation velocity of electromagnetic waves (light, in particular) in vacuum and called the speed of light. 3) is called the Minkowski metric tensor (the Minkowski metric). As usual, summing is assumed over repeated indices if one of them is covariant and the other contravariant.

The variation equation, as in Minkowski space, has the meaning of a trajectory (geodesic) equation, describing the extremum of the world line length between two given points. It can be written as duα µ ν + Γα µν u u = 0. 53) the general case, these differential equalities do not lead to integral conservation laws because, to do so, they should have the form ∂fµν /dxν = 0 , and it would be more precise to say that they express the SET change related to the metric change. 52), is often called conservative.

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Black Holes, Cosmology and Extra Dimensions by Kirill A Bronnikov


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