Lemaître coordinates are a particular set of coordinates for the Schwarzschild metric—a spherically symmetric solution to the Einstein field equations in vacuum—introduced by Georges Lemaître in 1932. Changing from Schwarzschild to Lemaître coordinates removes the coordinate singularity at the Schwarzschild radius.
Equations
The original Schwarzschild coordinate expression of the Schwarzschild metric, in natural units (), is given as
where
is the invariant interval; is the Schwarzschild radius; is the mass of the central body; are the Schwarzschild coordinates (which asymptotically turn into the flat spherical coordinates); is the speed of light; and is the gravitational constant.
This metric has a coordinate singularity at the Schwarzschild radius .
Georges Lemaître was the first to show that this is not a real physical singularity but simply a manifestation of the fact that the static Schwarzschild coordinates cannot be realized with material bodies inside the Schwarzschild radius. Indeed, inside the Schwarzschild radius everything falls towards the centre and it is impossible for a physical body to keep a constant radius.
A transformation of the Schwarzschild coordinate system from to the new coordinates
(the numerator and denominator are switched inside the square-roots), leads to the Lemaître coordinate expression of the metric,
where
The trajectories with ρ constant are timelike geodesics with τ the proper time along these geodesics. They represent the motion of freely falling particles which start out with zero velocity at infinity. At any point their speed is just equal to the escape velocity from that point.
In Lemaître coordinates the metric is non-singular at the Schwarzschild radius r=1, which instead corresponds to the point . However, there remains a genuine gravitational singularity at the center, where , which cannot be removed by a coordinate change.
The Lemaître coordinate system is synchronous, that is, the global time coordinate of the metric defines the proper time of co-moving observers. The radially falling bodies reach the Schwarzschild radius and the centre within finite proper time.
Along the trajectory of a radial light ray,
therefore no signal can escape from inside the Schwarzschild radius, where always and the light rays emitted radially inwards and outwards both end up at the origin. However the inward travelling rays come in from infinity and go to r=0 without singularity, while the outward travelling rays have go to infinity if starting from r<1, and originate from equals minus infinity at r=1 if heading out to infinite r. Ie, future travelling null rays are incomplete to the past. Although the metric is non-singular at r=1, all geodesics travelling away from r=1 are incomplete to the past with finite proper time between $r=1$ and any point outside r=1. ,
See also
Kruskal-Szekeres coordinates
Eddington–Finkelstein coordinates
Lemaître–Tolman metric
Introduction to the mathematics of general relativity
Stress–energy tensor
Metric tensor (general relativity) Relativistic angular momentum