Subrahmanyan Chandrasekhar (1910-1995). Indian-American astrophysicist who, as a nineteen-year-old on a steamship from India to Cambridge in 1930, calculated the upper mass limit beyond which a white dwarf star cannot stably exist — the Chandrasekhar limit, which determines whether a dying star ends as a white dwarf, a neutron star, or a black hole. The calculation was correct. The reception was hostile: Sir Arthur Eddington, then the dominant figure in British astrophysics, publicly ridiculed the result for years, and Chandrasekhar was effectively shut out of the British astrophysics community. He moved to the University of Chicago and spent a six-decade career producing foundational work in stellar structure, radiative transfer, general relativity, and black-hole physics. The Nobel Prize came in 1983, fifty-three years after the calculation that should have made him famous at twenty. His cognitive signature was monotropic deep work sustained across decades, willingness to wait out an integration apparatus that had refused to receive him, and a remarkable refusal of bitterness — he wrote eulogies for Eddington and continued to honor the older man's earlier contributions to astrophysics. The pattern: the integration apparatus eventually receives the discovery, but on its own schedule, often decades after the work was done.