Light rays too must follow geodesics in space-time. Again, the fact that space is curved means that light no longer appears to travel in straight lines in space. So general relativity predicts that light should be bent by gravitational fields. For example, the theory predicts that the light cones of points near the sun would be slightly bent inward, on account of the mass of the sun. This means that light from a distant star that happened to pass near the sun would be deflected through a small angle, causing the star to appear in a different position to an observer on the earth (Fig. 2.9). Of course, if the light from the star always passed close to the sun, we would not be able to tell whether the light was being deflected or if instead the star was really where we see it. However, as the earth orbits around the sun, different stars appear to pass behind the sun and have their light deflected. They therefore change their apparent position relative to other stars. It is normally very difficult to see this effect, because the light from the sun makes it impossible to observe stars that appear near to the sun the sky. However, it is possible to do so during an eclipse of the sun, when the sun’s light is blocked out by the moon.
Einstein’s prediction of light deflection could not be tested immediately in 1915, because the First World War was in progress, and it was not until 1919 that a British expedition, observing an eclipse from West Africa, showed that light was indeed deflected by the sun, just as predicted by the theory.
This proof of a German theory by British scientists was hailed as a great act of reconciliation between the two countries after the war. It is ionic, therefore, that later examination of the photographs taken on that expedition showed the errors were as great as the effect they were trying to measure.
Deflection 偏向
Reconciliation 調和
光線也必須沿著時空的測地線走。空間是彎曲的事實又一次意味著，在空間中光線看起來不是沿著直線走。這樣，廣義相對論預言光線必須被引力場所折彎。譬如，理論預言，由於太陽的質量的緣故，太陽近處的點的光錐會向內稍微偏折。這表明，從遠處恆星發出的剛好通過太陽附近的光線會被折彎很小的角度，對於地球上的觀察者而言，這恆星顯得是位於不同的位置（圖2.9）。當然，如果從恆星來的光線總是在靠太陽很近的地方穿過，則我們無從知道這光線是被偏折了，還是這恆星實際上就是在我們所看到的地方。然而，當地球繞著太陽公轉，不同的恆星從太陽後面通過，並且它們的光線被偏折。所以，相對於其他恆星而言，它們改變了表觀的位置。
在正常情況下，去觀察到這個效應是非常困難的，這是由於太陽的光線使得人們不可能觀看天空上出現在太陽附近的恆星。然而，在日食時就可能觀察到，這時太陽的光線被月亮遮住了。由於第一次世界大戰正在進行，愛因斯坦的光偏折的預言不可能在1915年立即得到驗證。直到1919年，一個英國的探險隊從西非觀測日食，指出光線確實像理論所預言的那樣被太陽所偏折。這次德國人的理論為英國人所證明被歡呼為戰後兩國和好的偉大行動。具有諷刺意味的是，後來人們檢查這回探險所拍的照片，發現其誤差和所企圖測量的效應同樣大。
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