Isaac Newton’s classical gravity ruled human science unchallenged for over two hundred years; Arthur Eddington photographed stars during a total solar eclipse and proved that the Sun’s heavy mass bends the path of light itself. Published in the Philosophical Transactions in 1920, this historic eclipse expedition verified General Relativity, overthrowing Newtonian physics and catapulting Albert Einstein into global fame.

In 1915, Albert Einstein completed his General Theory of Relativity, proposing that gravity is not a Newtonian invisible pulling force, but rather the physical bending and warping of spacetime around massive objects. To prove it, Einstein made a bold prediction: starlight passing close to the Sun during a total solar eclipse would be bent by exactly 1.75 arcseconds—twice what Newton’s theory predicted.
British astronomer Arthur Eddington traveled to the island of Príncipe during the May 1919 total eclipse. As the Moon blacked out the Sun's glare, Eddington photographed the stars of the Hyades cluster behind the Sun, confirming that the Sun’s gravitational warp had shifted the apparent position of the stars by the exact angle Einstein predicted.
The announcement in London made worldwide headlines: "Lights All Askew in the Heavens." By proving that spacetime is curved, by enabling modern gravitational lensing to map dark matter across the cosmos, and by founding modern cosmology, the 1919 eclipse expedition changed humanity’s picture of the universe.
IX. A determination of the deflection of light by the sun's gravitational field, from observations made at the total eclipse of May 29, 1919
1. The purpose of the expeditions was to determine what effect, if any, is produced by a gravitational field on the path of a ray of light traversing it. Apart from possible surprises, there appeared to be three alternatives, which it was especially desired to discriminate between— (1) The path is uninfluenced by gravitation. (2) The energy or mass of light is subject to gravitation in the same way as ordinary matter. If the law of gravitation is strictly the Newtonian law, this leads to an apparent displacement of a star close to the sun’s limb amounting to 0"·87 outwards. (3) The course of a, ray of light is in accordance with Einstein’s generalised relativity theory. This leads to an apparent displacement of a star at the limb amounting to 1"·75 outwards. In either of the last two cases the displacement is inversely proportional to the distance of the star from the sun’s centre, the displacement under (3) being just double the displacement under (2).
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