Josh Cryer: 1 revision

2009-01-21T11:02:33Z

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Jumpboy11j at 19:19, 4 December 2007

2007-12-04T19:19:41Z

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In physics and nuclear chemistry, nuclear fusion is the process by which multiple [[atom]]ic particles join together to form a heavier [[nucleus]]. It is accompanied by the release or absorption of [[energy]]. Iron and nickel nuclei have the largest binding energies per nucleon of all nuclei and therefore are the most stable. The fusion of two nuclei lighter than iron or nickel generally releases energy while the fusion of nuclei heavier than iron or nickel absorbs energy; vice-versa for the reverse process, [[nuclear fission]].

Nuclear fusion occurs naturally in [[star]]s. Artificial fusion in [[human]] enterprises has also been achieved, although not yet completely controlled. Building upon the nuclear transmutation experiments of Ernest Rutherford done a few years earlier, fusion of light nuclei ([[hydrogen]] [[isotope]]s) was first observed by Mark Oliphant in 1932, and the steps of the main cycle of nuclear fusion in stars were subsequently worked out by Hans Bethe throughout the remainder of that decade. Research into fusion for military purposes began in the early 1940s, as part of the [[Manhattan Project]], but was not successful until 1952. Research into controlled fusion for civilian purposes began in the 1950s, and continues to this day.

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Nuclear fusion - Revision history

Josh Cryer: 1 revision

Jumpboy11j at 19:19, 4 December 2007