Given a timelike unit vector field , Raychaudhuri's equation can be written where are quadratic invariants of the shear tensor and the vorticity tensor respectively. Here, is the expansion tensor, is its trace, called the expansion scalar, and is the projection tensor onto the hyperplanes orthogonal to. Also, dot denotes differentiation with respect toproper time counted along the world lines in the congruence. Finally, the trace of the tidal tensor can also be written as This quantity is sometimes called the Raychaudhuri scalar.
Intuitive significance
The expansion scalar measures the fractional rate at which the volume of a small ball of matter changes with respect to time as measured by a central comoving observer. In other words, the above equation gives us the evolution equation for the expansion of the timelike congruence. If the derivative of this quantity turns out to be negative along some world line, then any expansion of a small ball of matter must be followed by recollapse. If not, continued expansion is possible. The shear tensor measures any tendency of an initially spherical ball of matter to become distorted into an ellipsoidal shape. The vorticity tensor measures any tendency of nearby world lines to twist about one another. The right hand side of Raychaudhuri's equation consists of two types of terms:
terms which promote -collapse
* initially nonzero expansion scalar,
* nonzero shearing,
* positive trace of the tidal tensor; this is precisely the condition guaranteed by assuming the strong energy condition, which holds for the most important types of solutions, such as physically reasonable fluid solutions,
terms which oppose -collapse
* nonzero vorticity, corresponding to Newtonian centrifugal forces,
Usually one term will win out. However, there are situations in which a balance can be achieved. This balance may be:
stable: in the case of hydrostatic equilibrium of a ball of perfect fluid, the expansion, shear, and vorticity all vanish, and a radial divergence in the acceleration vector counteracts the Raychaudhuri scalar, which for a perfect fluid is in geometrized units. In Newtonian gravitation, the trace of the tidal tensor is ; in general relativity, the tendency of pressure to oppose gravity is partially offset by this term, which under certain circumstances can become important.
unstable: for example, the world lines of the dust particles in the Gödel solution have vanishing shear, expansion, and acceleration, but constant vorticity just balancing a constant Raychuadhuri scalar due to nonzero vacuum energy.
Focusing theorem
Suppose the strong energy condition holds in some region of our spacetime, and let be a timelike geodesic unit vector field with vanishing vorticity, or equivalently, which is hypersurface orthogonal. For example, this situation can arise in studying the world lines of the dust particles in cosmological models which are exact dust solutions of the Einstein field equation. Then Raychaudhuri's equation becomes Now the right hand side is always negative or zero, so the expansion scalar never increases in time. Since the last two terms are non-negative, we have Integrating this inequality with respect to proper time gives If the initial value of the expansion scalar is negative, this means that our geodesics must converge in a caustic within a proper time of at most after the measurement of the initial value of the expansion scalar. This need not signal an encounter with a curvature singularity, but it does signal a breakdown in our mathematical description of the motion of the dust.
Optical equations
There is also an optical version of Raychaudhuri's equation for null geodesic congruences. Here, the hats indicate that the expansion, shear and vorticity are only with respect to the transverse directions. When the vorticity is zero, then assuming the null energy condition, caustics will form before the affine parameter reaches.
Applications
The event horizon is defined as the boundary of the causal past of null infinity. Such boundaries are generated by null geodesics. The affine parameter goes to infinity as we approach null infinity, and no caustics form until then. So, the expansion of the event horizon has to be nonnegative. As the expansion gives the rate of change of the logarithm of the area density, this means the event horizon area can never go down, at least classically, assuming the null energy condition.
