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The light side of gravity

For the propagation of light, Einstein's theory makes a clear prediction: Light is deflected by gravity. Just as test particles move on the straightest-possible lines in curved space-time (i.e. on space-time geodesics), so does light.

The most basic example: Light rays passing a massive body are bent towards that mass. This effect increases for light rays that pass the body at smaller and smaller distances from it. The effect is shown in the following figure, with the massive body shown in yellow, and the light rays (with light moving from left to right) in red:

Lichtablenkung im Schwerefeld der Sonne


The first measurement of this relativistic effect was made by British astronomers in 1919. They used the fact that light deflection changes astronomical observations. The "location of a star in the night sky" is simply short-hand for "the direction from which that star's light reaches us". Starlight that passes close to the sun before reaching us gets deflected, as sketched in the figure above (but by a much smaller amount than is shown there). This starlight will thus reach us from a slightly different direction than when the sun is in some different region of the sky. Accordingly, the star's position in the night sky is shifted slightly.

Under ordinary circumstances, the disk of the sun is much too bright for astronomers to observe nearby stars. But during a solar eclipse, such observations are possible, and that's what two British expeditions did in 1919: They traveled to locations from which they could observe a solar eclipse, photographed the stars near the sun, and compared these images with photographs taken of that same region of the sky while the sun was somewhere else. The comparison confirmed Einstein's predictions (although, in these early measurements, not to any great precision). In the wake of those observations, general relativity became a theory to be reckoned with (and Einstein became the celebrity he still is today).

An important application of the deflection effect concerns so-called gravitational lenses, masses configured in a way that astronomers can see two or more images of one and the same far-away object in the night-sky! The following photograph shows a famous example. No, those aren't four objects forming a cross around the center - they're four images of one and the same object:


Einsteinkreuz, Aufnahme des HST

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