An introduction to mathematical cosmology by J. N. Islam

By J. N. Islam

This booklet presents a concise creation to the mathematical elements of the starting place, constitution and evolution of the universe. The e-book starts with a quick assessment of observational and theoretical cosmology, in addition to a quick advent of basic relativity. It then is going directly to talk about Friedmann versions, the Hubble consistent and deceleration parameter, singularities, the early universe, inflation, quantum cosmology and the far-off 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 area via quite a few theoretical and observational constraints, and provides a brand new inflationary answer for a 6th measure capability. This booklet is acceptable as a textbook for complicated undergraduates and starting graduate scholars. it is going to even be of curiosity to cosmologists, astrophysicists, utilized mathematicians and mathematical physicists.

Show description

Read Online or Download An introduction to mathematical cosmology PDF

Best cosmology books

From the Universe to the Elementary Particles: A First Introduction to Cosmology and the Fundamental Interactions (Undergraduate Lecture Notes in Physics)

During this ebook, the writer leads the reader, step-by-step and with none complicated arithmetic, to a transparent figuring out of the principles of contemporary effortless particle physics and cosmology. He additionally addresses present and debatable questions about issues akin to string concept. The e-book contains gentle introductions to the theories of specified and common relativity, and likewise classical and quantum box conception.

Universe of Fluctuations

The failure of all makes an attempt to unify gravitation with different primary interactions has bring about an abandonment of element debris and differentiable spacetime of normal Relativity and Quantum conception, together with Quantum box conception. whereas Quantum Superstrings (or M-Theory) and different Quantum Gravity ways paintings with a lattice like constitution or prolonged items, a number of unanswered questions stay.

Astronomy and Cosmogony

This moment variation, initially released in 1929, is an intensive survey on the leading edge of cosmology and astronomy with specific connection with the actual kingdom of topic, the constitution, composition and life-cycle of stars, and the superstructures of nebulae and galaxies. meant as a rigourously argued clinical treatise, each attempt used to be made by means of denims to render the result of far-reaching developments in cosmology intelligible to a large diversity of readers.

Extra resources for An introduction to mathematical cosmology

Example text

An equivalent description, known as Weyl’s postulate (Weyl, 1923) is to assume that the worldlines of galaxies are a bundle or congruence of geodesics in space-time diverging from a point in the (finite or infinitely distant) past, or converging to such a point in the future, or both. These geodesics are non-intersecting, except possibly at a singular point in the past or future or both. There is one and only one such geodesic passing through each regular (that is, a point which is not a singularity) space-time point.

32), the ‘radius’ of this sphere, that is, the distance from the ‘centre’ given by ␺ ϭ0 to the surface given by ␺ ϭ ␺0 along ␪ ϭ constant and ␾ ϭconstant, is R␺0. Thus the surface area is larger than that of a sphere of radius R␺0 in Euclidean space. In this case the range of the coordinates (␺, ␪, ␾) is: 0ഛ ␺ ഛϱ,0ഛ ␪ ഛ ␲, 0ഛ ␾ Ͻ 2␲. The spatial volume is infinite. 3 Some kinematic properties of the Robertson–Walker metric We have seen that galaxies have fixed spatial coordinates, that is, they are at rest in the coordinate system defined above.

The circumference of the circle on the sphere given by ␺Јϭconstantϭ ␺Ј0 is 2␲RЈ sin␺Ј0, while the distance of this circle from the north pole O is RЈ␺Ј0. The circumference of this circle reaches a maximum at ␺0Ј ϭ ␲/2, after which it decreases until it reaches zero at ␺Ј0 ϭ ␲, when the distance from the north pole along the surface is RЈ␲, analogously to the previous case. 24), the entire surface is swept by the coordinate range 0ഛ ␺ ഛ ␲, 0 ഛ ␪ ഛ ␲, 0 ഛ ␾ ഛ2␲. 20) is 44 The Robertson–Walker metric RЈsincЈ0 RЈ cЈ0 cЈϭp/2 Fig.

Download PDF sample

Rated 4.91 of 5 – based on 43 votes