Odd number theorem explained

The odd number theorem is a theorem in strong gravitational lensing which comes directly from differential topology.

The theorem states that the number of multiple images produced by a bounded transparent lens must be odd.

Formulation

The gravitational lensing is a thought to mapped from what's known as image plane to source plane following the formula :

M:(u,v)\mapsto(u',v')

.

Argument

If we use direction cosines describing the bent light rays, we can write a vector field on

(u,v)

plane

V:(s,w)

.

However, only in some specific directions

V0:(s0,w0)

, will the bent light rays reach the observer, i.e., the images only form where

D=\delta

V=0|
(s0,w0)
. Then we can directly apply the Poincaré–Hopf theorem

\chi=\sumindexD=constant

.

The index of sources and sinks is +1, and that of saddle points is -1. So the Euler characteristic equals the difference between the number of positive indices

n+

and the number of negative indices

n-

. For the far field case, there is only one image, i.e.,

\chi=n+-n-=1

. So the total number of images is

N=n++n-=2n-+1

, i.e., odd. The strict proof needs Uhlenbeck's Morse theory of null geodesics.

References

This article is licensed under the GNU Free Documentation License. It uses material from the Wikipedia article "Odd number theorem".

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