Добавил:
Upload Опубликованный материал нарушает ваши авторские права? Сообщите нам.
Вуз: Предмет: Файл:
FREGRAVOL2.pdf
Скачиваний:
71
Добавлен:
05.06.2015
Размер:
8.65 Mб
Скачать

108

5 Cosmology and General Relativity

relevant role in higher dimensional gravitational theories like those that emerge in supergravity and superstring theory.

Next, introducing also isotropy, we go over to the standard cosmological model and to its back-bone that are Friedman equations. The latter are analyzed in all respects and consequences, discussing the role of the spatial curvature, the available types of hydrodynamical equations of state and the exact solutions that are known for them, corresponding to various energy fillings of the Universe. Particular attention is paid to the embedding of cosmological metrics within de Sitter space.

After discussing horizons and the conceptual problem of homogeneous initial boundary conditions we go over to discuss the mathematical modeling of the inflationary scenario by means of the coupling of gravity to a scalar field, endowed with a potential. The general framework of the slow rolling phase is presented together with examples of numerical solutions of the coupled Einstein-Klein-Gordon equations.

The next addressed topic is perturbations. We discuss in detail the general form of the scalar perturbations in the coupled Einstein-Klein-Gordon system and we derive the form of the independent scalar degree of freedom which we canonically quantize. In this way we are able to outline the derivation of the power spectrum of the primeval quantum fluctuations that is currently experimentally observed in the anisotropies of the Cosmic Microwave Background. The relation between the fluctuations of the radiation temperature T and those of the gravitational quantized potential Φ is due to the so called Sachs Wolfe effect whose derivation we also present.

5.2Mathematical Interlude: Isometries and the Geometry of Coset Manifolds

The existence of continuous isometries is related with the existence of Killing vector fields which we already utilized in various occasions. Now we have to explain the underlying mathematical theory in full and this leads us to introduce a relevant chapter of differential geometry which is the study of coset manifolds and symmetric spaces. The present section is devoted to these topics.

5.2.1 Isometries and Killing Vector Fields

Finite isometries of a (pseudo-)Riemannian manifold Mg are diffeomorphisms:

φ : M M

(5.2.1)

such that their pull-back1 on the metric form leaves it invariant:

φ gμν (x) dxμ dxν = gμν (x) dxμ dxν

(5.2.2)

1See Sect. 3.3 of Volume 1 for the definition of the pull-back and of the push-forward.

5.2 Mathematical Interlude: Isometries and the Geometry of Coset Manifolds

109

Suppose now that the considered diffeomorphism is infinitesimally close to the identity:

xμ φμ(x) xμ + kμ(x)

(5.2.3)

The condition for this diffeomorphism to be an isometry, is a differential equation for the components of the vector field k = kμμ which immediately follows from (5.2.2):

μkν + ν kμ = 0

(5.2.4)

Hence given a metric one can investigate the nature of its isometries by trying to solve the linear homogeneous equations (5.2.4) determining its general integral. The important point is that, if we have two Killing vectors k and w also their commutator [k, w] will be a Killing vector. This follows from the fact that the product of two finite isometries is also an isometry. Hence Killing vector fields form a finite dimensional Lie algebra Giso and one can turn the question around. Rather then calculating the isometries of a given metric one can address the problem of constructing (pseudo-)Riemannian manifolds that have a prescribed isometry algebra. Due to the well established classification of semi-simple Lie algebras this becomes a very fruitful point of view.

In particular, also in view of the Cosmological Principle, one is interested in homogeneous spaces, namely in (pseudo-)Riemannian manifolds where each point of the manifold can be reached from a reference one by the action of an isometry.

Homogeneous spaces are identified with coset manifolds, whose differential geometry can be thoroughly described and calculated in pure Lie algebra terms.

5.2.2 Coset Manifolds

Coset manifolds are a natural generalization of group manifolds and play a very important, ubiquitous, role both in Mathematics and in Physics.

In group-theory (irrespectively whether the group G is finite or infinite, continuous or discrete) we have the concept of coset space G/H which is just the set of equivalence classes of elements g G, where the equivalence is defined by right multiplication with elements h H G of a subgroup:

g, g G : g g iff h H \ gh = g

(5.2.5)

Namely two group elements are equivalent if and only if they can be mapped into each other by means of some element of the subgroup. The equivalence classes, which constitute the elements of G/H are usually denoted gH, where g is any representative of the class, namely any one of the equivalent G-group elements the class is composed of. The definition we have just provided by means of right multiplication can be obviously replaced by an analogous one based on left-multiplication. In this case we construct the coset H\G composed of right lateral classes Hg while gH

110

5 Cosmology and General Relativity

are named the left lateral classes. For non-Abelian groups G and generic subgroups H the left G/H and right H\G coset spaces have different not coinciding elements. Working with one or with the other definition is just a matter of conventions. We choose to work with left classes.

Coset manifolds arise in the context of Lie group theory when G is a Lie group and H is a Lie subgroup thereof. In that case the set of lateral classes gH can be endowed with a manifold structure inherited from the manifold structure of the parent group G. Furthermore on G/H we can construct invariant metrics such that all elements of the original group G are isometries of the constructed metric. As we show below, the curvature tensor of invariant metrics on coset manifolds can be constructed in purely algebraic terms starting from the structure constants of the G Lie algebra, by-passing all analytic differential calculations.

The reason why coset manifolds are relevant to Cosmology is encoded in the concept of homogeneity, that is one of the two pillars of the Cosmological Principle. Indeed coset manifolds are easily identified with homogeneous spaces which we presently define.

Definition 5.2.1 A Riemannian or pseudo-Riemannian manifold Mg is said to be homogeneous if it admits as an isometry the transitive action of a group G. A group acts transitively if any point of the manifold can be reached from any other by means of the group action.

A notable and very common example of such homogeneous manifolds is pro-

vided by the spheres Sn and by their non-compact generalizations, the pseudospheres H(n± +1m,m). Let xI denote the Cartesian coordinates in Rn+1 and let:

ηI J = diag(+, + . . . , +, , , . . . , )

(5.2.6)

 

 

 

 

 

 

 

 

 

 

 

 

+

 

 

 

 

n

 

 

1m

m

 

be the coefficient of a non-degenerate quadratic form with signature (n + 1 m, m):

x, x!η xI xJ ηI J

(5.2.7)

We obtain a pseudo-sphere H(n± +1m,m) by defining the algebraic locus:

x

 

H(n+1m,m)

 

x, x

!η ≡ ±

1

(5.2.8)

 

±

 

 

 

which is a manifold of dimension n. The spheres Sn correspond to the particular case Hn++1,0 where the quadratic form is positive definite and the sign in the right hand side of (5.2.8) is positive. Obviously with a positive definite quadratic form this is the only possibility.

All these algebraic loci are invariant under the transitive action of the group SO(n + 1, n + 1 m) realized by matrix multiplication on the vector x since:

g G : x, x!η = ±1 gx, gx!η = ±1

(5.2.9)

5.2 Mathematical Interlude: Isometries and the Geometry of Coset Manifolds

111

namely the group maps solutions of the constraint (5.2.8) into solutions of the same and, furthermore, all solutions can be generated starting from a standard reference vector:

x, x

!η

= ±

1

 

 

 

g

 

\ =

 

0

(5.2.10)

 

 

 

 

 

 

 

 

G x

 

gx±

where:

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

1

 

 

 

 

 

 

 

 

0

 

 

 

 

 

 

0

 

 

 

 

 

 

0

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

0

 

 

 

 

 

 

0

 

 

x

+

 

 

 

 

x

 

 

 

 

 

(5.2.11)

 

 

 

 

 

 

 

0

 

;

 

 

0

 

 

 

 

 

 

 

 

=

0

 

 

 

 

 

=

1

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

0

 

 

 

 

 

 

 

 

0

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

.

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

0

 

 

 

 

 

 

 

 

0

 

 

 

the line separating the first n + 1 m entries from the last m. Equation (5.2.10) guarantees that the locus is invariant under the action G, while (5.2.11) states that G is transitive.

Definition 5.2.2 In a homogeneous space Mg , the subgroup Hp G which leaves a point p Mg fixed ( h Hp , hp = p) is named the isotropy subgroup of the point. Because of the transitive action of G, any other point p = gp has an isotropy subgroup Hp = gHpg1 which is conjugate to Hp and therefore isomorphic to it.

It follows that, up to conjugation, the isotropy group of a homogeneous manifold Mg is unique and corresponds to an intrinsic property of such a space. It suffices to calculate the isotropy group H0 of a conventional properly chosen reference point p0: all other isotropy groups will immediately follow. For brevity H0 will be just

renamed H.

In our example of the spaces H(n± +1m,m) the isotropy group is immediately derived by looking at the form of the vectors x±0 : all elements of G which rotate the vanishing entries of these vectors among themselves are clearly elements of the isotropy group. Hence we find:

H

=

SO(n, m)

 

for H(n+1m,m)

 

 

 

 

 

 

+

(5.2.12)

H

=

SO(n

+

1, m

1) for H(n+1m,m)

 

 

 

 

 

It is natural to label any point p of a homogeneous space by the parameters describing the G-group element which carries a conventional point p0 into p. These parameters, however, are redundant: because of the H-isotropy there are infinitely many ways to reach p from p0. Indeed, if g does that job, any other element of the lateral class gH does the same. It follows by this simple discussion that the homogeneous manifold Mg can be identified with the coset manifold G/H defined by the transitive group G divided by the isotropy group H.

112

5 Cosmology and General Relativity

Focusing once again on our example we find:

H(n+1m,m)

=

SO(n + 1 m, m)

;

+

SO(n

m, m)

 

In particular the spheres correspond to:

H(n+1m,m)

SO(n + 1 m, m)

= SO(n + 1 m, m 1)

 

(5.2.13)

Sn = H(n+1,0) =

SO(n + 1)

(5.2.14)

SO(n)

+

 

Other important examples, relevant for cosmology are:

H(n+1,1)

=

SO(n + 1, 1)

;

H(n+1,1)

=

SO(n + 1, 1)

(5.2.15)

 

+

SO(n, 1)

SO(n

+

1)

 

 

 

The general classification of homogeneous (pseudo-)Riemannian spaces corresponds therefore to the classification of the coset manifolds G/H for all Lie groups G and for their closed Lie subgroups H G.

The equivalence classes constituting the points of the coset manifold can be labeled by a set of d coordinates y ≡ {y1, . . . , yd } where:

G

dim G dim H

 

d = dim H

(5.2.16)

There are of course many different ways of choosing the y-parameters since, just as in any other manifold, there are many possible coordinate systems. What is specific of coset manifolds is that, given any coordinate system y by means of which we label the equivalence classes, within each equivalence class we can choose a representative group element L(y) G. The choice must be done in such a way that L(y) should be a smooth function of the parameters y. Furthermore for different values y and y , the group elements L(y) and L(y ) should never be equivalent, in other words no h H should exist such that L(y) = L(y )h. Under left multiplication by g G, L(y) is in general carried into another equivalence class with coset representative L(y ). Yet the g image of L(y) is not necessarily L(y ): it is typically some other element of the same class, so that we can write:

g G : gL(y) = L y h(g, y); h(g, y) H

(5.2.17)

where we emphasized that the H-element necessary to map L(y ) into the g-image of L(y), depends, in general both from the point y and from the chosen transformation g. Equation (5.2.17) is pictorially described in Fig. 5.1. For the spheres a possible set of coordinates y can be obtained by means of the stereographic projection described, for the case of the two-sphere, in chapter two of Volume 1. Its conception is recalled here in Fig. 5.2.

As an other explicit example, which will be useful in the sequel, we consider the case of the Euclidian hyperbolic spaces H(n,1) identified as coset manifolds in (5.2.15). In this case, to introduce a coset parameterization means to write a family of SO(n, 1) matrices L(y) depending smoothly on an n-component vector y

5.2 Mathematical Interlude: Isometries and the Geometry of Coset Manifolds

113

Fig. 5.1 Pictorial description of the action of the group G on the coset representatives

in such a way that for different values of y such matrices cannot be mapped one in the other by means of right multiplication with any element h of the subgroup SO(n) SO(n, 1):

SO(n, 1) SO(n) # h =

O

0

;

O

T

O = 1n×n

(5.2.18)

0

1

 

An explicit parameterization of this type can be written as follows:

L(y)

 

1n×n

+ 2 1y2

 

2 1y2

 

(5.2.19)

 

=

 

 

 

 

yyT

 

 

y

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

2 1y y2

 

1+y2

 

 

 

 

 

T

 

1 y2

 

 

 

 

 

 

where y2 y · y denotes the standard SO(n) invariant scalar product in Rn. Why the matrices L(y) form a good parameterization of the coset? The reason is simple, first of all observe that:

L(y)T ηL(y) = η

(5.2.20)

Fig. 5.2 The idea of the stereographic projection. Considering the Sn sphere immersed in Rn+1, from the North-Pole {1, 0, 0, . . . , 0} one draws the line that goes through the point p Sn and considers the point π(p) Rn where such a line intersects the Rn plane tangent to sphere in the South Pole and orthogonal to the line that joins the North and the South Pole. The n-coordinates {y1, . . . , yn} of π(p) can be taken as labels of an open chart in Sn

Соседние файлы в предмете [НЕСОРТИРОВАННОЕ]