- •Preface
- •Acknowledgements
- •Contents
- •2.1 Introduction and a Short History of Black Holes
- •2.2 The Kruskal Extension of Schwarzschild Space-Time
- •2.2.1 Analysis of the Rindler Space-Time
- •2.2.2 Applying the Same Procedure to the Schwarzschild Metric
- •2.2.3 A First Analysis of Kruskal Space-Time
- •2.3 Basic Concepts about Future, Past and Causality
- •2.3.1 The Light-Cone
- •2.3.2 Future and Past of Events and Regions
- •Achronal Sets
- •Time-Orientability
- •Domains of Dependence
- •Cauchy surfaces
- •2.4.1 Conformal Mapping of Minkowski Space into the Einstein Static Universe
- •2.4.2 Asymptotic Flatness
- •2.5 The Causal Boundary of Kruskal Space-Time
- •References
- •3.1 Introduction
- •3.2 The Kerr-Newman Metric
- •3.2.1 Riemann and Ricci Curvatures of the Kerr-Newman Metric
- •3.3 The Static Limit in Kerr-Newman Space-Time
- •Static Observers
- •3.4 The Horizon and the Ergosphere
- •The Horizon Area
- •3.5 Geodesics of the Kerr Metric
- •3.5.2 The Hamilton-Jacobi Equation and the Carter Constant
- •3.5.3 Reduction to First Order Equations
- •3.5.4 The Exact Solution of the Schwarzschild Orbit Equation as an Application
- •3.5.5 About Explicit Kerr Geodesics
- •3.6 The Kerr Black Hole and the Laws of Thermodynamics
- •3.6.1 The Penrose Mechanism
- •3.6.2 The Bekenstein Hawking Entropy and Hawking Radiation
- •References
- •4.1 Historical Introduction to Modern Cosmology
- •4.2 The Universe Is a Dynamical System
- •4.3 Expansion of the Universe
- •4.3.1 Why the Night is Dark and Olbers Paradox
- •4.3.2 Hubble, the Galaxies and the Great Debate
- •4.3.4 The Big Bang
- •4.4 The Cosmological Principle
- •4.5 The Cosmic Background Radiation
- •4.6 The New Scenario of the Inflationary Universe
- •4.7 The End of the Second Millennium and the Dawn of the Third Bring Great News in Cosmology
- •References
- •5.1 Introduction
- •5.2 Mathematical Interlude: Isometries and the Geometry of Coset Manifolds
- •5.2.1 Isometries and Killing Vector Fields
- •5.2.2 Coset Manifolds
- •5.2.3 The Geometry of Coset Manifolds
- •5.2.3.1 Infinitesimal Transformations and Killing Vectors
- •5.2.3.2 Vielbeins, Connections and Metrics on G/H
- •5.2.3.3 Lie Derivatives
- •5.2.3.4 Invariant Metrics on Coset Manifolds
- •5.2.3.5 For Spheres and Pseudo-Spheres
- •5.3 Homogeneity Without Isotropy: What Might Happen
- •5.3.1 Bianchi Spaces and Kasner Metrics
- •5.3.1.1 Bianchi Type I and Kasner Metrics
- •5.3.2.1 A Ricci Flat Bianchi II Metric
- •5.3.3 Einstein Equation and Matter for This Billiard
- •5.3.4 The Same Billiard with Some Matter Content
- •5.3.5 Three-Space Geometry of This Toy Model
- •5.4 The Standard Cosmological Model: Isotropic and Homogeneous Metrics
- •5.4.1 Viewing the Coset Manifolds as Group Manifolds
- •5.5 Friedman Equations for the Scale Factor and the Equation of State
- •5.5.1 Proof of the Cosmological Red-Shift
- •5.5.2 Solution of the Cosmological Differential Equations for Dust and Radiation Without a Cosmological Constant
- •5.5.3 Embedding Cosmologies into de Sitter Space
- •5.6 General Consequences of Friedman Equations
- •5.6.1 Particle Horizon
- •5.6.2 Event Horizon
- •5.6.3 Red-Shift Distances
- •5.7 Conceptual Problems of the Standard Cosmological Model
- •5.8 Cosmic Evolution with a Scalar Field: The Basis for Inflation
- •5.8.1 de Sitter Solution
- •5.8.2 Slow-Rolling Approximate Solutions
- •5.8.2.1 Number of e-Folds
- •5.9 Primordial Perturbations of the Cosmological Metric and of the Inflaton
- •5.9.1 The Conformal Frame
- •5.9.2 Deriving the Equations for the Perturbation
- •5.9.2.1 Meaning of the Propagation Equation
- •5.9.2.2 Evaluation of the Effective Mass Term in the Slow Roll Approximation
- •5.9.2.3 Derivation of the Propagation Equation
- •5.9.3 Quantization of the Scalar Degree of Freedom
- •5.9.4 Calculation of the Power Spectrum in the Two Regimes
- •5.9.4.1 Short Wave-Lengths
- •5.9.4.2 Long Wave-Lengths
- •5.9.4.3 Gluing the Long and Short Wave-Length Solutions Together
- •5.9.4.4 The Spectral Index
- •5.10 The Anisotropies of the Cosmic Microwave Background
- •5.10.1 The Sachs-Wolfe Effect
- •5.10.2 The Two-Point Temperature Correlation Function
- •5.10.3 Conclusive Remarks on CMB Anisotropies
- •References
- •6.1 Historical Outline and Introduction
- •6.1.1 Fermionic Strings and the Birth of Supersymmetry
- •6.1.2 Supersymmetry
- •6.1.3 Supergravity
- •6.2 Algebro-Geometric Structure of Supergravity
- •6.3 Free Differential Algebras
- •6.3.1 Chevalley Cohomology
- •Contraction and Lie Derivative
- •Definition of FDA
- •Classification of FDA and the Analogue of Levi Theorem: Minimal Versus Contractible Algebras
- •6.4 The Super FDA of M Theory and Its Cohomological Structure
- •6.4.1 The Minimal FDA of M-Theory and Cohomology
- •6.4.2 FDA Equivalence with Larger (Super) Lie Algebras
- •6.5 The Principle of Rheonomy
- •6.5.1 The Flow Chart for the Construction of a Supergravity Theory
- •6.6 Summary of Supergravities
- •Type IIA Super-Poicaré Algebra in the String Frame
- •The FDA Extension of the Type IIA Superalgebra in the String Frame
- •The Bianchi Identities
- •6.7.1 Rheonomic Parameterizations of the Type IIA Curvatures in the String Frame
- •Bosonic Curvatures
- •Fermionic Curvatures
- •6.7.2 Field Equations of Type IIA Supergravity in the String Frame
- •6.8 Type IIB Supergravity
- •SL(2, R) Lie Algebra
- •Coset Representative of SL(2, R)/O(2) in the Solvable Parameterization
- •The SU(1, 1)/U(1) Vielbein and Connection
- •6.8.2 The Free Differential Algebra, the Supergravity Fields and the Curvatures
- •The Curvatures of the Free Differential Algebra in the Complex Basis
- •The Curvatures of the Free Differential Algebra in the Real Basis
- •6.8.3 The Bosonic Field Equations and the Standard Form of the Bosonic Action
- •6.9 About Solutions
- •References
- •7.1 Introduction and Conceptual Outline
- •7.2 p-Branes as World Volume Gauge-Theories
- •7.4 The New First Order Formalism
- •7.4.1 An Alternative to the Polyakov Action for p-Branes
- •7.6 The D3-Brane: Summary
- •7.9 Domain Walls in Diverse Space-Time Dimensions
- •7.9.1 The Randall Sundrum Mechanism
- •7.9.2 The Conformal Gauge for Domain Walls
- •7.10 Conclusion on This Brane Bestiary
- •References
- •8.1 Introduction
- •8.2 Supergravity and Homogeneous Scalar Manifolds G/H
- •8.2.3 Scalar Manifolds of Maximal Supergravities in Diverse Dimensions
- •8.3 Duality Symmetries in Even Dimensions
- •8.3.1 The Kinetic Matrix N and Symplectic Embeddings
- •8.3.2 Symplectic Embeddings in General
- •8.5 Summary of Special Kähler Geometry
- •8.5.1 Hodge-Kähler Manifolds
- •8.5.2 Connection on the Line Bundle
- •8.5.3 Special Kähler Manifolds
- •8.6 Supergravities in Five Dimension and More Scalar Geometries
- •8.6.1 Very Special Geometry
- •8.6.3 Quaternionic Geometry
- •8.6.4 Quaternionic, Versus HyperKähler Manifolds
- •References
- •9.1 Introduction
- •9.2 Black Holes Once Again
- •9.2.2 The Oxidation Rules
- •Orbit of Solutions
- •The Schwarzschild Case
- •The Extremal Reissner Nordström Case
- •Curvature of the Extremal Spaces
- •9.2.4 Attractor Mechanism, the Entropy and Other Special Geometry Invariants
- •9.2.5 Critical Points of the Geodesic Potential and Attractors
- •At BPS Attractor Points
- •At Non-BPS Attractor Points of Type I
- •At Non-BPS Attractor Points of Type II
- •9.2.6.2 The Quartic Invariant
- •9.2.7.1 An Explicit Example of Exact Regular BPS Solution
- •The Metric
- •The Scalar Field
- •The Electromagnetic Fields
- •The Fixed Scalars at Horizon and the Entropy
- •The Metric
- •The Scalar Field
- •The Electromagnetic Fields
- •The Fixed Scalars at Horizon and the Entropy
- •9.2.9 Resuming the Discussion of Critical Points
- •Non-BPS Case
- •BPS Case
- •9.2.10 An Example of a Small Black Hole
- •The Metric
- •The Complex Scalar Field
- •The Electromagnetic Fields
- •The Charges
- •Structure of the Charges and Attractor Mechanism
- •9.2.11 Behavior of the Riemann Tensor in Regular Solutions
- •9.3.4 The SO(8) Spinor Bundle and the Holonomy Tensor
- •9.3.5 The Well Adapted Basis of Gamma Matrices
- •9.3.6 The so(8)-Connection and the Holonomy Tensor
- •9.3.7 The Holonomy Tensor and Superspace
- •9.3.8 Gauged Maurer Cartan 1-Forms of OSp(8|4)
- •9.3.9 Killing Spinors of the AdS4 Manifold
- •9.3.10 Supergauge Completion in Mini Superspace
- •9.3.11 The 3-Form
- •9.4.1 Maurer Cartan Forms of OSp(6|4)
- •9.4.2 Explicit Construction of the P3 Geometry
- •9.4.3 The Compactification Ansatz
- •9.4.4 Killing Spinors on P3
- •9.4.5 Gauge Completion in Mini Superspace
- •9.4.6 Gauge Completion of the B[2] Form
- •9.5 Conclusions
- •References
- •10.1 The Legacy of Volume 1
- •10.2 The Story Told in Volume 2
- •Appendix A: Spinors and Gamma Matrix Algebra
- •A.2 The Clifford Algebra
- •A.2.1 Even Dimensions
- •A.2.2 Odd Dimensions
- •A.3 The Charge Conjugation Matrix
- •A.4 Majorana, Weyl and Majorana-Weyl Spinors
- •Appendix B: Auxiliary Tools for p-Brane Actions
- •B.1 Notations and Conventions
- •Appendix C: Auxiliary Information About Some Superalgebras
- •C.1.1 The Superalgebra
- •C.2 The Relevant Supercosets and Their Relation
- •C.2.1 Finite Supergroup Elements
- •C.4 An so(6) Inversion Formula
- •Appendix D: MATHEMATICA Package NOVAMANIFOLDA
- •Coset Manifolds (Euclidian Signature)
- •Instructions for the Use
- •Description of the Main Commands of RUNCOSET
- •Structure Constants for CP2
- •Spheres
- •N010 Coset
- •RUNCOSET Package (Euclidian Signature)
- •Main
- •Spin Connection and Curvature Routines
- •Routine Curvapack
- •Routine Curvapackgen
- •Contorsion Routine for Mixed Vielbeins
- •Calculation of the Contorsion for General Manifolds
- •Calculation for Cartan Maurer Equations and Vielbein Differentials (Euclidian Signature)
- •Routine Thoft
- •AdS Space in Four Dimensions (Minkowski Signature)
- •Lie Algebra of SO(2, 3) and Killing Metric
- •Solvable Subalgebra Generating the Coset and Construction of the Vielbein
- •Killing Vectors
- •Trigonometric Coordinates
- •Test of Killing Vectors
- •MANIFOLDPROVA
- •The 4-Dimensional Coset CP2
- •Calculation of the (Pseudo-)Riemannian Geometry of a Kasner Metric in Vielbein Formalism
- •References
- •Index
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 = kμ∂μ 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± +1−m,m). Let xI denote the Cartesian coordinates in Rn+1 and let:
ηI J = diag(+, + . . . , +, −, −, . . . , −) |
(5.2.6) |
|||||||||
|
|
|
|
|
|
|
|
|
|
|
|
+ |
|
|
|
||||||
|
n |
|
|
1−m |
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± +1−m,m) by defining the algebraic locus:
x |
|
H(n+1−m,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 = gHpg−1 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± +1−m,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+1−m,m) |
|
||
|
|
|
|
|
+ |
(5.2.12) |
|
H |
= |
SO(n |
+ |
1, m |
− |
1) for H(n+1−m,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+1−m,m) |
= |
SO(n + 1 − m, m) |
; |
||
+ |
SO(n |
− |
m, m) |
||
|
In particular the spheres correspond to:
H(n+1−m,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 1−y2 |
|
−2 1−y2 |
|
(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