1. The problem statement, all variables and given/known data This is for my intro to General Relativity class, using Hartle's text Gravity: An intro to Einstein's GR. 12.1 "How many protons must combine to make one He nuclei every second to provide the luminosity of the Sun? Estimate how long the Sun could go on at this rate before all its protons were used up." 2. Relevant equations L = 3.85×1026J/s The hint given by the professor, probably to save us from attempting to use the actual thermonuclear fusion chain: 4H → 4He 3. The attempt at a solution At first I thought this may be a 4-vector and CM frame problem, but the reaction equation didn't include a γ term that would represent light carrying away energy. I decided to take an overly simple approximation heavy route, and ended up with 6.8×1045 protons fused per second and a corresponding Solar lifetime of 4160 years which is obviously ridiculous. My method was: 75% of the sun is H therefore: 8.92×1056 H atoms available for fusion let n = #fusions/second nγ = L Approximating γ as the blackbody peak of 1.41eV (from Daniel V. Schroeder's Thermal Physics) n ≈ 1.7×1045 fusions/second = 6.8×1045 protons fused/second Then it follows that the lifetime of the sun t, is: t ≈ 1.31×1011 seconds ≈ 4160 yrs. This does not seem like the approach I was supposed to take and is a ridiculous answer, but there was nothing on luminosity in the chapter as it is mostly on the Schwarzchild black hole and Kruskal-Szekeres coordinates. If I am supposed to use 4-vector methods, where do I get the released energy from given that the reaction is 4H → 4He?