Lemaitre-Tolman metric

The spherically symmetric dust solution of Einstein's field equations was first found by Lemaitre 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 "Lemaitre-Tolman-Bondi metric" and the "Tolman metric".

The metric is::
$mathrm\{d\}s^\{2\}\; =\; mathrm\{d\}t^2\; -\; frac\{(R\text{'})^2\}\{1\; -\; 2\; E\}\; mathrm\{d\}r^2\; -\; R^2\; ,\; mathrm\{d\}Omega^2$

where::
$mathrm\{d\}Omega^2\; =\; mathrm\{d\}\; heta^2\; +\; sin^2\; heta\; ,\; mathrm\{d\}phi^2$
:
$R\; =\; R(t,r)~,~~~~~~~~\; R\text{'}\; =\; partial\; R\; /\; partial\; r~,~~~~~~~~\; E\; =\; E(r)$

The matter is comoving, which means its 4-velocity is::
$u^a\; =\; delta^a\_0\; =\; (1,\; 0,\; 0,\; 0)$
so the spatial coordinates $(r,\; heta,\; phi)$ are attached to the particles of dust.

The pressure is zero (hence "dust"), the density is :
$8\; pi\; ho\; =\; frac\{2\; M\text{'}\}\{R^2\; ,\; R\text{'}\}$
and the evolution equation is:
$dot\{R\}^2\; =\; frac\{2\; M\}\{R\}\; +\; 2\; E$
where:
$dot\{R\}\; =\; partial\; R\; /\; partial\; t$

The evolution equation has three solutions, depending on the sign of $E$,:
$E\; >\; 0:~~~~~~~~\; R\; =\; frac\{M\}\{2\; E\}\; (cosheta\; -\; 1)~,~~~~~~~~\; (sinheta\; -\; eta)\; =\; frac\{(2\; E)^\{3/2\}\; (t\; -\; t\_B)\}\{M\}~;$
:
$E\; =\; 0:~~~~~~~~\; R\; =\; left(\; frac\{9\; M\; (t\; -\; a)^2\}\{2\}\; ight)^\{1/3\}~;$
:

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 $r$,

$t\_B(r)$ - the time of the big bang for worldlines at radius $r$.

Special cases are the Schwarzschild metric in geodesic coordinates$M\; =$ constant, and the Robertson-Walker metric $E\; propto\; M^\{2/3\}~,~~\; t\_B\; =$ constant.

References

* Lemaitre, G., Ann. Soc. Sci. Bruxelles, A53, 51 (1933).
* Tolman, R.C., Proc. Natl. Acad. Sci. 20, 169 (1934).
* Bondi, H., Mon. Not. R. Astron. Soc. 107, 410 (1947).
* Krasinski, A., "Inhomogeneous Cosmological Models", (1997) Cambridge UP, ISBN 0 521 48180 5