Spacetime symmetries: Difference between revisions

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{{Expert-subject|Mathematics|date=November 2008}}
{{Expert-subject|Mathematics|date=November 2008}}
{{for|the notation|Ricci calculus}}
'''Spacetime symmetries''' are features of [[spacetime]] that can be described as exhibiting some form of [[symmetry]]. The role of [[symmetry in physics]] is important in simplifying solutions to many problems, spacetime symmetries finding ample application in the study of [[exact solutions]] of [[Einstein's field equations]] of [[general relativity]].
'''Spacetime symmetries''' are features of [[spacetime]] that can be described as exhibiting some form of [[symmetry]]. The role of [[symmetry in physics]] is important in simplifying solutions to many problems, spacetime symmetries finding ample application in the study of [[exact solutions]] of [[Einstein's field equations]] of [[general relativity]].


==Physical motivation==
==Physical motivation==


Physical problems are often investigated and solved by noticing features which have some form of symmetry. For example, in the [[Schwarzschild solution]], the role of [[spherically symmetric spacetime|spherical symmetry]] is important in [[deriving the Schwarzschild solution]] and deducing the physical consequences of this symmetry (such as the non-existence of gravitational radiation in a spherically pulsating star). In cosmological problems, symmetry finds a role to play in the [[cosmological principle]] which restricts the type of universes that are consistent with large-scale observations (e.g. the [[Friedmann-Lemaitre-Robertson-Walker metric|Friedmann-Lemaitre-Robertson-Walker (FLRW) metric]]). Symmetries usually require some form of preserving property, the most important of which in general relativity include the following:
Physical problems are often investigated and solved by noticing features which have some form of symmetry. For example, in the [[Schwarzschild solution]], the role of [[spherically symmetric spacetime|spherical symmetry]] is important in [[deriving the Schwarzschild solution]] and deducing the physical consequences of this symmetry (such as the non-existence of gravitational radiation in a spherically pulsating star). In cosmological problems, symmetry finds a role to play in the [[cosmological principle]] which restricts the type of universes that are consistent with large-scale observations (e.g. the [[Friedmann–Lemaître–Robertson–Walker metric|Friedmann-Lemaître-Robertson-Walker (FLRW) metric]]). Symmetries usually require some form of preserving property, the most important of which in general relativity include the following:


*preserving geodesics of the spacetime
*preserving geodesics of the spacetime
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==Mathematical definition==
==Mathematical definition==


A rigorous definition of symmetries in general relativity has been given by Hall (2004). In this approach, the idea is to use (smooth) [[vector fields]] whose [[local diffeomorphism|local flow diffeomorphisms]] preserve some property of the [[spacetime]]. This preserving property of the diffeomorphisms is made precise as follows. A smooth vector field <math>X</math> on a spacetime <math>M</math> is said to '''preserve''' a smooth tensor <math>T</math> on <math>M</math> (or <math>T</math> is '''invariant''' under <math>X</math>) if, for each smooth local flow diffeomorphism <math>\phi_t</math> associated with <math>X</math>, the tensors <math>T</math> and <math>\phi_t{}^*(T)</math> are equal on the domain of <math>\phi_t</math>. This statement is equivalent to the more usable condition that the [[Lie derivative]] of the [[tensor]] under the vector field vanishes:
A rigorous definition of symmetries in general relativity has been given by Hall (2004). In this approach, the idea is to use (smooth) [[vector fields]] whose [[local diffeomorphism|local flow diffeomorphisms]] preserve some property of the [[spacetime]]. This preserving property of the diffeomorphisms is made precise as follows. A smooth vector field ''X'' on a spacetime ''M'' is said to ''preserve'' a smooth tensor ''T'' on ''M'' (or ''T'' is '''invariant''' under ''X'') if, for each smooth local flow diffeomorphism ''ϕ<sub>t</sub>'' associated with ''X'', the tensors ''T'' and ''ϕ''<sub>''t''</sub>*(''T'') are equal on the domain of ''ϕ<sub>t</sub>''. This statement is equivalent to the more usable condition that the [[Lie derivative]] of the [[tensor]] under the vector field vanishes:


:<math>\mathcal{L}_X T=0</math>
:<math>\mathcal{L}_X T=0</math>


on <math>M</math>. This has the consequence that, given any two points <math>p</math> and <math>q</math> on <math>M</math>, the coordinates of <math>T</math> in a coordinate system around <math>p</math> are equal to the coordinates of <math>T</math> in a coordinate system around <math>q</math>. A '''''symmetry on the spacetime''''' is a smooth vector field whose local flow diffeomorphisms preserve some (usually geometrical) feature of the spacetime. The (geometrical) feature may refer to specific tensors (such as the metric, or the energy-momentum tensor) or to other aspects of the spacetime such as its geodesic structure. The vector fields are sometimes referred to as '''''collineations''''', '''''symmetry vector fields''''' or just '''''symmetries'''''. The set of all symmetry vector fields on <math>M</math> forms a [[Lie algebra]] under the [[Lie bracket]] operation as can be seen from the identity:  
on ''M''. This has the consequence that, given any two points ''p'' and ''q'' on ''M'', the coordinates of ''T'' in a coordinate system around ''p'' are equal to the coordinates of ''T'' in a coordinate system around ''q''. A ''symmetry on the spacetime'' is a smooth vector field whose local flow diffeomorphisms preserve some (usually geometrical) feature of the spacetime. The (geometrical) feature may refer to specific tensors (such as the metric, or the energy-momentum tensor) or to other aspects of the spacetime such as its geodesic structure. The vector fields are sometimes referred to as ''collineations'', ''symmetry vector fields'' or just ''symmetries''. The set of all symmetry vector fields on ''M'' forms a [[Lie algebra]] under the [[Lie_bracket_of_vector_fields|Lie bracket]] operation as can be seen from the identity:  


: <math>\mathcal{L}_{[X,Y]} T = \mathcal{L}_X (\mathcal{L}_Y T) - \mathcal{L}_Y (\mathcal{L}_X T)</math>
: <math>\mathcal{L}_{[X,Y]} T = \mathcal{L}_X (\mathcal{L}_Y T) - \mathcal{L}_Y (\mathcal{L}_X T)</math>
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:<math>\mathcal{L}_X g_{ab}=\phi g_{ab}</math>
:<math>\mathcal{L}_X g_{ab}=\phi g_{ab}</math>


where <math>\phi</math> is a smooth real-valued function on <math>M</math>.
where ''ϕ'' is a smooth real-valued function on <math>M</math>.


==Curvature symmetry==
==Curvature symmetry==
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:<math>\mathcal{L}_X R^a{}_{bcd}=0</math>
:<math>\mathcal{L}_X R^a{}_{bcd}=0</math>


where <math>R^a{}_{bcd}</math> are the components of the Riemann tensor. The [[Set (mathematics)|set]] of all [[smooth function|smooth]] curvature collineations forms a [[Lie algebra]] under the [[Lie bracket]] operation (if the smoothness condition is dropped, the set of all curvature collineations need not form a Lie algebra). The Lie algebra is denoted by <math>CC(M)</math> and may be [[infinity|infinite]]-[[dimension]]al. Every affine vector field is a curvature collineation.
where ''R<sup>a</sup><sub>bcd</sub>'' are the components of the Riemann tensor. The [[Set (mathematics)|set]] of all [[smooth function|smooth]] curvature collineations forms a [[Lie algebra]] under the [[Lie bracket]] operation (if the smoothness condition is dropped, the set of all curvature collineations need not form a Lie algebra). The Lie algebra is denoted by ''CC''(''M'') and may be [[infinity|infinite]]-[[dimension]]al. Every affine vector field is a curvature collineation.


==Matter symmetry==
==Matter symmetry==
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:<math>\mathcal{L}_X T_{ab}=0</math>
:<math>\mathcal{L}_X T_{ab}=0</math>


where <math>T_{ab}</math> are the energy-momentum tensor components. The intimate relation between geometry and physics may be highlighted here, as the vector field <math>X</math> is regarded as preserving certain physical quantities along the flow lines of <math>X</math>, this being true for any two observers. In connection with this, it may be shown that ''every Killing vector field is a matter collineation'' (by the Einstein field equations, with or without [[cosmological constant]]). Thus, given a solution of the EFE, ''a vector field that preserves the metric necessarily preserves the corresponding energy-momentum tensor''. When the energy-momentum tensor represents a perfect fluid, every Killing vector field preserves the energy density, pressure and the fluid flow vector field. When the energy-momentum tensor represents an electromagnetic field, a Killing vector field does ''not necessarily'' preserve the electric and magnetic fields.
where ''T<sub>ab</sub>'' are the energy-momentum tensor components. The intimate relation between geometry and physics may be highlighted here, as the vector field ''X'' is regarded as preserving certain physical quantities along the flow lines of ''X'', this being true for any two observers. In connection with this, it may be shown that ''every Killing vector field is a matter collineation'' (by the Einstein field equations, with or without [[cosmological constant]]). Thus, given a solution of the EFE, ''a vector field that preserves the metric necessarily preserves the corresponding energy-momentum tensor''. When the energy-momentum tensor represents a perfect fluid, every Killing vector field preserves the energy density, pressure and the fluid flow vector field. When the energy-momentum tensor represents an electromagnetic field, a Killing vector field does ''not necessarily'' preserve the electric and magnetic fields.


==Local and global symmetries==
==Local and global symmetries==
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As mentioned at the start of this article, the main application of these symmetries occur in general relativity, where solutions of Einstein's equations may be classified by imposing some certain symmetries on the spacetime.
As mentioned at the start of this article, the main application of these symmetries occur in general relativity, where solutions of Einstein's equations may be classified by imposing some certain symmetries on the spacetime.


=== Spacetime Classifications ===
=== Spacetime classifications ===


Classifying solutions of the EFE constitutes a large part of general relativity research. Various approaches to classifying spacetimes, including using the [[Segre classification]] of the energy-momentum tensor or the [[Petrov classification]] of the [[Weyl tensor]] have been studied extensively by many researchers, most notably Stephani et al. (2003). They also classify spacetimes using symmetry vector fields (especially Killing and homothetic symmetries). For example, Killing vector fields may be used to classify spacetimes, as there is a limit to the number of global, smooth Killing vector fields that a spacetime may possess (the maximum being 10 for 4-dimensional spacetimes). Generally speaking, the higher the dimension of the algebra of symmetry vector fields on a spacetime, the more symmetry the spacetime admits. For example, the Schwarzschild solution has a Killing algebra of dimension 4 (3 spatial rotational vector fields and a time translation), whereas the [[Friedmann-Lemaitre-Robertson-Walker metric|Friedmann-Lemaitre-Robertson-Walker (FLRW) metric]] (excluding the [[Einstein static]] subcase) has a Killing algebra of dimension 6 (3 translations and 3 rotations). The Einstein static metric has a Killing algebra of dimension 7 (the previous 6 plus a time translation).
Classifying solutions of the EFE constitutes a large part of general relativity research. Various approaches to classifying spacetimes, including using the [[Segre classification]] of the energy-momentum tensor or the [[Petrov classification]] of the [[Weyl tensor]] have been studied extensively by many researchers, most notably Stephani et al. (2003). They also classify spacetimes using symmetry vector fields (especially Killing and homothetic symmetries). For example, Killing vector fields may be used to classify spacetimes, as there is a limit to the number of global, smooth Killing vector fields that a spacetime may possess (the maximum being 10 for 4-dimensional spacetimes). Generally speaking, the higher the dimension of the algebra of symmetry vector fields on a spacetime, the more symmetry the spacetime admits. For example, the Schwarzschild solution has a Killing algebra of dimension 4 (3 spatial rotational vector fields and a time translation), whereas the [[Friedmann–Lemaître–Robertson–Walker metric|Friedmann-Lemaître-Robertson-Walker (FLRW) metric]] (excluding the [[Einstein static]] subcase) has a Killing algebra of dimension 6 (3 translations and 3 rotations). The Einstein static metric has a Killing algebra of dimension 7 (the previous 6 plus a time translation).


The assumption of a spacetime admitting a certain symmetry vector field can place restrictions on the spacetime.
The assumption of a spacetime admitting a certain symmetry vector field can place restrictions on the spacetime.


=== Form of the Metric ===
== See also ==
== See also ==


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*[[Ricci decomposition]]
*[[Ricci decomposition]]
*[[Symmetry in physics]]
*[[Symmetry in physics]]
*[[Symmetry in quantum mechanics]]
*[[Derivations of the Lorentz transformations]]


==References==
==References==

Revision as of 13:06, 28 August 2013

Template:Expert-subject

{{#invoke:Hatnote|hatnote}}

Spacetime symmetries are features of spacetime that can be described as exhibiting some form of symmetry. The role of symmetry in physics is important in simplifying solutions to many problems, spacetime symmetries finding ample application in the study of exact solutions of Einstein's field equations of general relativity.

Physical motivation

Physical problems are often investigated and solved by noticing features which have some form of symmetry. For example, in the Schwarzschild solution, the role of spherical symmetry is important in deriving the Schwarzschild solution and deducing the physical consequences of this symmetry (such as the non-existence of gravitational radiation in a spherically pulsating star). In cosmological problems, symmetry finds a role to play in the cosmological principle which restricts the type of universes that are consistent with large-scale observations (e.g. the Friedmann-Lemaître-Robertson-Walker (FLRW) metric). Symmetries usually require some form of preserving property, the most important of which in general relativity include the following:

  • preserving geodesics of the spacetime
  • preserving the metric tensor
  • preserving the curvature tensor

These and other symmetries will be discussed in more detail later. This preservation feature can be used to motivate a useful definition of symmetries.

Mathematical definition

A rigorous definition of symmetries in general relativity has been given by Hall (2004). In this approach, the idea is to use (smooth) vector fields whose local flow diffeomorphisms preserve some property of the spacetime. This preserving property of the diffeomorphisms is made precise as follows. A smooth vector field X on a spacetime M is said to preserve a smooth tensor T on M (or T is invariant under X) if, for each smooth local flow diffeomorphism ϕt associated with X, the tensors T and ϕt*(T) are equal on the domain of ϕt. This statement is equivalent to the more usable condition that the Lie derivative of the tensor under the vector field vanishes:

on M. This has the consequence that, given any two points p and q on M, the coordinates of T in a coordinate system around p are equal to the coordinates of T in a coordinate system around q. A symmetry on the spacetime is a smooth vector field whose local flow diffeomorphisms preserve some (usually geometrical) feature of the spacetime. The (geometrical) feature may refer to specific tensors (such as the metric, or the energy-momentum tensor) or to other aspects of the spacetime such as its geodesic structure. The vector fields are sometimes referred to as collineations, symmetry vector fields or just symmetries. The set of all symmetry vector fields on M forms a Lie algebra under the Lie bracket operation as can be seen from the identity:

the term on the right usually being written, with an abuse of notation, as .

Killing symmetry

{{#invoke:main|main}} A Killing vector field is one of the most important types of symmetries and is defined to be a smooth vector field that preserves the metric tensor:

This is usually written in the expanded form as:

Killing vector fields find extensive applications (including in classical mechanics) and are related to conservation laws.

Homothetic symmetry

{{#invoke:main|main}} A homothetic vector field is one which satisfies:

where c is a real constant. Homothetic vector fields find application in the study of singularities in general relativity.

Affine symmetry

{{#invoke:main|main}} An affine vector field is one that satisfies:

An affine vector field preserves geodesics and preserves the affine parameter.

The above three vector field types are special cases of projective vector fields which preserve geodesics without necessarily preserving the affine parameter.

Conformal symmetry

{{#invoke:main|main}} A conformal vector field is one which satisfies:

where ϕ is a smooth real-valued function on .

Curvature symmetry

{{#invoke:main|main}} A curvature collineation is a vector field which preserves the Riemann tensor:

where Rabcd are the components of the Riemann tensor. The set of all smooth curvature collineations forms a Lie algebra under the Lie bracket operation (if the smoothness condition is dropped, the set of all curvature collineations need not form a Lie algebra). The Lie algebra is denoted by CC(M) and may be infinite-dimensional. Every affine vector field is a curvature collineation.

Matter symmetry

{{#invoke:main|main}} A less well-known form of symmetry concerns vector fields that preserve the energy-momentum tensor. These are variously referred to as matter collineations or matter symmetries and are defined by:

where Tab are the energy-momentum tensor components. The intimate relation between geometry and physics may be highlighted here, as the vector field X is regarded as preserving certain physical quantities along the flow lines of X, this being true for any two observers. In connection with this, it may be shown that every Killing vector field is a matter collineation (by the Einstein field equations, with or without cosmological constant). Thus, given a solution of the EFE, a vector field that preserves the metric necessarily preserves the corresponding energy-momentum tensor. When the energy-momentum tensor represents a perfect fluid, every Killing vector field preserves the energy density, pressure and the fluid flow vector field. When the energy-momentum tensor represents an electromagnetic field, a Killing vector field does not necessarily preserve the electric and magnetic fields.

Local and global symmetries

Template:Empty section

Applications

As mentioned at the start of this article, the main application of these symmetries occur in general relativity, where solutions of Einstein's equations may be classified by imposing some certain symmetries on the spacetime.

Spacetime classifications

Classifying solutions of the EFE constitutes a large part of general relativity research. Various approaches to classifying spacetimes, including using the Segre classification of the energy-momentum tensor or the Petrov classification of the Weyl tensor have been studied extensively by many researchers, most notably Stephani et al. (2003). They also classify spacetimes using symmetry vector fields (especially Killing and homothetic symmetries). For example, Killing vector fields may be used to classify spacetimes, as there is a limit to the number of global, smooth Killing vector fields that a spacetime may possess (the maximum being 10 for 4-dimensional spacetimes). Generally speaking, the higher the dimension of the algebra of symmetry vector fields on a spacetime, the more symmetry the spacetime admits. For example, the Schwarzschild solution has a Killing algebra of dimension 4 (3 spatial rotational vector fields and a time translation), whereas the Friedmann-Lemaître-Robertson-Walker (FLRW) metric (excluding the Einstein static subcase) has a Killing algebra of dimension 6 (3 translations and 3 rotations). The Einstein static metric has a Killing algebra of dimension 7 (the previous 6 plus a time translation).

The assumption of a spacetime admitting a certain symmetry vector field can place restrictions on the spacetime.

See also

References

  • {{#invoke:citation/CS1|citation

|CitationClass=book }} See Section 10.1 for a definition of symmetries.

  • {{#invoke:citation/CS1|citation

|CitationClass=book }}

  • {{#invoke:citation/CS1|citation

|CitationClass=book }} See Chapter 3 for properties of the Lie derivative and Section 3.10 for a definition of invariance.