In the first of three papers I wrote in 1905, I examined a phenomenon that had been known for some years, but unexplained. I called it the 'Photoelectric Effect'. Electromagnetic energy, previously thought to be 'waves', seemed to be emitted in small bundles called 'photons'. My explanation, and my guess that the energy of a photon was related to its frequency by the equation E = hv, this is what I earned my only Nobel Prize for. My second 1905 paper proposed what is today called the special theory of relativity. I based my new theory on a reinterpretation of the classical principle of relativity, namely that the laws of physics had to have the same form in any frame of reference. Secondly, I assumed that the speed of light remained constant in all frames of reference. This was a brand new way of looking at things, redefining the 'absolute' ideas first proposed by Isaac Newton, and it was the foundation for my General Theory of Relativity, which I would complete some 10 years later. Still in 1905, I proposed an explanation for the equivalence of energy and matter, describing his most famous equation E=mc². After 1905, I continued to work on my ideas, attempting to extend my special theory of relativity to explain what happens when objects accelerate. In 1909, I became a professor of physics at the University of Bern. In 1911, I predicted that if my theories were true, light rays from distant stars passing near the very massive sun would be bent due to gravitational attraction. This prediction was confirmed in 1919, during a solar eclipse. I began my work on the General Theory of Relativity in 1912, with the help of several mathematicians. This explanation of how gravity works, published in 1915, became the foundation for modern relativistic physics, and laid the groundwork for our current knowledge about black holes. When British eclipse expeditions in 1919 confirmed my predictions, I became famous. The New York Times ran the headline on November 10th, 1919: