Abstract

The deformation retract of the Kerr spacetime is introduced using Lagrangian equations. The equatorial geodesics of the Kerr space have been discussed. The retraction of this space into itself and into geodesics has been presented. The deformation retract of this space into itself and after the isometric folding has been discussed. Theorems concerning these relations have been deduced.

1. Introduction

The real revolution in mathematical physics in the second half of twentieth century (and in pure mathematics itself) was algebraic topology and algebraic geometry [1]. In the nineteenth century, mathematical physics was essentially the classical theory of ordinary and partial differential equations. The variational calculus, as a basic tool for physicists in theoretical mechanics, was seen with great reservation by mathematicians until Hilbert set up its rigorous foundation by pushing forward functional analysis. This marked the transition into the first half of twentieth century, where, under the influence of quantum mechanics and relativity, mathematical physics turned mainly into functional analysis, complemented by the theory of Lie groups and by tensor analysis. All branches of theoretical physics still can expect the strongest impacts of use of the unprecedented wealth of results of algebraic topology and algebraic geometry of the second half of the twentieth century [1].

Today, the concepts and methods of topology and geometry have become an indispensable part of theoretical physics. They have led to a deeper understanding of many crucial aspects in condensed matter physics, cosmology, gravity, and particle physics. Moreover, several intriguing connections between only apparently disconnected phenomena have been revealed based on these mathematical tools [2, 3].

Topology enters general relativity through the fundamental assumption that spacetime exists and is organized as a manifold. This means that spacetime has a well-defined dimension, but it also carries with it the inherent possibility of modified patterns of global connectivity, such as distinguishing a sphere from a plane or a torus from a surface of higher genus. Such modifications can be present in the spatial topology without affecting the time direction, but they can also have a genuine spacetime character in which case the spatial topology changes with time [4]. The topology change in classical general relativity has been discussed in [5]. See [6] for some applications of differential topology in general relativity.

In general relativity, boundaries that are bundles over some compact manifolds arise in gravitational thermodynamics [7]. The trivial bundle is a classic example. Manifolds with complete Ricci-flat metrics admitting such boundaries are known; they are the Euclideanised Schwarzschild metric and the flat metric with periodic identification. York [8] shows that there are in general two or no Schwarzschild solutions depending on whether the squashing (the ratio of the radius of the -fibre to that of the -base) is below or above a critical value. York’s results in 4-dimension extend readily to higher dimensions.

The simplest example of nontrivial bundles arises in quantum cosmology in which the boundary is a compact , that is, a nontrivial bundle over . In the case of zero cosmological constant, regular 4 metrics admitting such an boundary are the Taub-Nut [9] and Taub-Bolt [10] metrics having zero and two-dimensional (regular) fixed point sets of the action, respectively [7, 11–13].

The Kerr metric describes the geometry of empty spacetime around a rotating uncharged axially symmetric black hole. The Kerr metric corresponds to the line element

The parameter , termed the Kerr parameter, has units of length in geometrized units. The parameter will be interpreted as angular momentum and the parameter will be interpreted as the mass for the black hole. The Kerr metric is a vacuum solution of the Einstein equations, being valid in the absence of matter. If the black hole is not rotating , the Kerr line element reduces to the Schwarzschild line element. The Kerr metric becomes asymptotically flat for and . Unlike the Schwarzschild metric, the Kerr metric has only axial symmetry.

2. Deformation Retract

2.1. Deformation Retract Definitions

The theory of deformation retract is very interesting topic in Euclidean and non-Euclidean spaces. It has been investigated from different points of view in many branches of topology and differential geometry. A retraction is a continuous mapping from the entire space into a subspace which preserves the position of all points in that subspace [14].

(i) Let and be two smooth manifolds of dimensions and , respectively. A map is said to be an isometric folding of into if and only if, for every piecewise geodesic path , the induced path is a piecewise geodesic and of the same length as [15]. If does not preserve the lengths, it is called topological folding. Many types of foldings are discussed in [16–21]. Some applications are discussed in [22, 23].

(ii) A subset of a topological space is called a retraction of if there exists a continuous map such that [24] (a) is open; (b) , .

(iii) A subset of a topological space is said to be a deformation retract if there exist a retraction and a homotopy such that [24]

The deformation retract is a particular case of homotopy equivalence and two spaces are homotopy equivalent if and only if they are both deformation retracts of a single larger space.

Deformation retracts of Stein spaces have been studied in [25]. The deformation retract of the 4D Schwarzschild metric has been discussed in [26] where it was found that the retraction of the Schwarzschild space is spacetime geodesic. The 5-dimensional case has been discussed in [27].

3. Equatorial Geodesics

We will be interested in the equatorial geodesics, that is, geodesics with . It is easy to show that such geodesics exist for the case of Kerr metric where satisfies the -component of the Euler Lagrange equations for the Lagrangian associated with the Kerr metric (1). Consider

The -component of the Euler Lagrange equations gives

Comparing the Kerr line element, And the four-dimensional flat metric

The coordinates of the four-dimensional Kerr space (6) can be written as

In general relativity, the geodesic equation is equivalent to the Euler Lagrange equations associated to the Lagrangian

To find a geodesic which is a subset of the Kerr space, the Lagrangian could be written as

There is no explicit dependence on or ; thus and are constants of motion; that is,

So we have the following set of equations:

If the constant is zero, we have

Since which is the great circle in the Kerr space , this geodesic is a retraction in Kerr space; . This is a retraction.

For , (12) becomes If , then . If the constant is zero, then

Since which is the great circle in the Kerr space , this geodesic is a retraction in Kerr space; .

If , then If the constant is zero, then

Since which is the great circle in the Kerr space , this geodesic is a retraction in Kerr space; .

From the above discussion, the following theorem has been proved.

Theorem 1. The retraction of the Kerr space is a geodesic in the Kerr space.

4. Deformation Retract of Kerr Space

The deformation retract of the Kerr space is defined as where is the closed interval . The retraction of the Kerr space is defined as

Then, the deformation retract of the Kerr space into a geodesic is defined by where

The deformation retract of the Kerr space into a geodesic is defined by

The deformation retract of the Kerr space into a geodesic is defined by

Now we are going to discuss the folding of the Kerr space : where

An isometric folding of the Kerr space into itself may be defined by

The deformation retract of the folded Kerr space into the folded is with