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{{general relativity}}
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{{no footnotes|date=January 2012}}
{{Technical|date=August 2011|reason=This article is great if one is a mathematician.  This is an interesting metric that really needs an expert's touch to explain it.  P. Ellsworth, ed.}}
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In mathematical physics, the '''Lemaître–Tolman metric''' is the spherically symmetric dust solution of [[Einstein's field equations]] was first found by [[Georges Lemaître|Lemaître]] in 1933 and then [[Richard Tolman|Tolman]] in 1934.  It was later investigated by [[Hermann Bondi|Bondi]] in 1947.  This solution describes a spherical cloud of dust (finite or infinite) that is expanding or collapsing under gravity. It is also known as the '''Lemaître-Tolman-Bondi metric''' and the '''Tolman metric'''.
 
The metric is:
: <math>\mathrm{d}s^{2} = \mathrm{d}t^2 - \frac{(R')^2}{1 + 2 E} \mathrm{d}r^2 - R^2 \, \mathrm{d}\Omega^2</math>
 
where:
: <math>\mathrm{d}\Omega^2 = \mathrm{d}\theta^2 + \sin^2\theta \, \mathrm{d}\phi^2</math></center>
: <math>R = R(t,r)~,~~~~~~~~ R' = \partial R / \partial r~,~~~~~~~~ E = E(r)</math>
 
The matter is comoving, which means its 4-velocity is:
: <math>u^a = \delta^a_0 = (1, 0, 0, 0)</math>
so the spatial coordinates <math>(r, \theta, \phi)</math> are attached to the particles of dust.
 
The pressure is zero (hence ''dust''), the density is  
: <math>8 \pi \rho = \frac{2 M'}{R^2 \, R'}</math>
and the evolution equation is
: <math>\dot{R}^2 = \frac{2 M}{R} + 2 E</math>
where
: <math>\dot{R} = \partial R / \partial t</math>
 
The evolution equation has three solutions, depending on the sign of <math>E</math>,
: <math>E > 0:~~~~~~~~ R = \frac{M}{2 E} (\cosh\eta - 1)~,~~~~~~~~ (\sinh\eta - \eta) = \frac{(2 E)^{3/2} (t - t_B)}{M}~;</math>
: <math>E = 0:~~~~~~~~ R = \left( \frac{9 M (t - t_B)^2}{2} \right)^{1/3}~;</math>
: <math>E < 0:~~~~~~~~ R = \frac{M}{2 E} (1 - \cos\eta)~,~~~~~~~~ (\eta - \sin\eta) = \frac{(-2 E)^{3/2} (t - t_B)}{M}~;</math>
which are known as ''hyperbolic'', ''parabolic'', and ''elliptic'' evolutions respectively.
 
The meanings of the three arbitrary functions, which depend on <math>r</math> only, are:
* <math>E(r)</math> – both a local geometry parameter, and the energy per unit mass of the dust particles at comoving coordinate radius <math>r</math>,
* <math>M(r)</math> – the gravitational mass within the comoving sphere at radius <math>r</math>,
* <math>t_B(r)</math> – the time of the big bang for worldlines at radius <math>r</math>.
 
Special cases are the [[Schwarzschild metric]] in [[geodesic coordinate]]s
<math>M =</math> constant, and the [[Friedmann–Lemaître–Robertson–Walker metric]], e.g. <math>E = 0~,~~ t_B =</math> constant for the flat case.
 
==See also==
 
*[[Lemaître coordinates]]
*[[Introduction to the mathematics of general relativity]]
*[[Stress–energy tensor]]
*[[Metric tensor (general relativity)]]
*[[Relativistic angular momentum]]
 
== References ==
 
* {{cite journal | last =Bondi | first =Hermann | authorlink =Hermann Bondi | coauthors = | title =Spherically symmetrical models in general relativity | journal =Monthly Notices of the Royal Astronomical Society | volume =107 | issue = | pages =410 | publisher = | location = | year =1947 | issn = | doi = | id =  | archiveurl= | archivedate= | bibcode =1947MNRAS.107..410B }}
* Krasinski, A., ''Inhomogeneous Cosmological Models'', (1997) Cambridge UP, ISBN 0-521-48180-5
* Lemaitre, G., Ann. Soc. Sci. Bruxelles, A53, 51 (1933).
* {{cite journal | last =Tolman | first =Richard C. | authorlink =Richard C. Tolman | coauthors = | title =Effect of Inhomogeneity on Cosmological Models | journal =Proc.  Natl. Acad.  Sci. | volume =20 | issue =3 | pages =169 | publisher =National Academy of Sciences of the USA | location = | year =1934 | url =http://www.pnas.org/content/20/3/169.full.pdf | issn = | doi = | id = | accessdate =2011-01-27 | archiveurl=http://www.webcitation.org/5w35fIoge | archivedate=2011-01-27 | pmid =16587869 | pmc =1076370 }}
 
{{relativity-stub}}
 
{{DEFAULTSORT:Lemaitre-Tolman metric}}
 
[[Category:Metric tensors]]
[[Category:Spacetime]]
[[Category:Coordinate charts in general relativity]]
[[Category:General relativity]]
[[Category:Gravitation]]
[[Category:Exact solutions in general relativity]]

Revision as of 03:18, 17 March 2013

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In mathematical physics, the Lemaître–Tolman metric is the spherically symmetric dust solution of Einstein's field equations was first found by Lemaître in 1933 and then Tolman in 1934. It was later investigated by Bondi in 1947. This solution describes a spherical cloud of dust (finite or infinite) that is expanding or collapsing under gravity. It is also known as the Lemaître-Tolman-Bondi metric and the Tolman metric.

The metric is:

ds2=dt2(R)21+2Edr2R2dΩ2

where:

dΩ2=dθ2+sin2θdϕ2
R=R(t,r),R=R/r,E=E(r)

The matter is comoving, which means its 4-velocity is:

ua=δ0a=(1,0,0,0)

so the spatial coordinates (r,θ,ϕ) are attached to the particles of dust.

The pressure is zero (hence dust), the density is

8πρ=2MR2R

and the evolution equation is

R˙2=2MR+2E

where

R˙=R/t

The evolution equation has three solutions, depending on the sign of E,

E>0:R=M2E(coshη1),(sinhηη)=(2E)3/2(ttB)M;
E=0:R=(9M(ttB)22)1/3;
E<0:R=M2E(1cosη),(ηsinη)=(2E)3/2(ttB)M;

which are known as hyperbolic, parabolic, and elliptic evolutions respectively.

The meanings of the three arbitrary functions, which depend on r only, are:

  • E(r) – both a local geometry parameter, and the energy per unit mass of the dust particles at comoving coordinate radius r,
  • M(r) – the gravitational mass within the comoving sphere at radius r,
  • tB(r) – the time of the big bang for worldlines at radius r.

Special cases are the Schwarzschild metric in geodesic coordinates M= constant, and the Friedmann–Lemaître–Robertson–Walker metric, e.g. E=0,tB= constant for the flat case.

See also

References

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