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George William Hill (3 de marzo de 1838 – 16 de abril, de 1914) fue un astrónomo y matemático estadounidense . Semblanza. Hill nació en Nueva York, y se trasladó con su familia a West Nyack cuando tenía ocho años. Después de asistir a la escuela secundaria, Hill se graduó por la Universidad de Rutgers en 1859.
George William Hill (March 3, 1838 – April 16, 1914) was an American astronomer and mathematician. Working independently and largely in isolation from the wider scientific community, he made major contributions to celestial mechanics and to the theory of ordinary differential equations.
12 de abr. de 2024 · Subjects Of Study: Moon. planet. space motion. George William Hill (born March 3, 1838, New York City, New York, U.S.—died April 16, 1914, West Nyack, New York) was an American mathematical astronomer considered by many of his peers to be the greatest master of celestial mechanics of his time.
- The Editors of Encyclopaedia Britannica
George William Hill (3 de marzo de 1838 - 16 de abril de 1914) fue un astrónomo y matemático estadounidense. Trabajando de forma independiente y en gran medida aislado de la comunidad científica en general, hizo importantes contribuciones a la mecánica celeste y a la teoría de las ecuaciones diferenciales ordinarias.
George William Hill. Quick Info. Born. 3 March 1838. New York, USA. Died. 16 April 1914. West Nyack, New York, USA. Summary. George Hill was an American astronomer and mathematician. who worked on the three-body problem and later on the four-body problem. View two larger pictures. Biography.
Hill Center for Mathematical Sciences, Rutgers University. George William Hill Professorship of Mathematics and Physics, Rutgers University. Bibliography. After earning a B.A. at Rutgers, G.W. Hill joined the staff of the Nautical Almanac Office in Cambridge, Massachusetts, in 1861.
(1838–1914) Americanmathematician and astronomer. Inspired by the work of L. Euler, he developed advanced mathematical methods for tackling problems in dynamical astronomy. His first major work was an application of the three-body problem: the orbits of Jupiter and Saturn and the perturbations exerted by these planets on the Moon.
