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nuclear chemistry - Wood County Schools
nuclear chemistry - Wood County Schools

... protons and neutrons in the nucleus. Below is a sample nuclear reaction, the decay of uranium-238 to thorium-234: Notice that the top numbers are conserved: 238 = 4 + 234. The bottom numbers are as well: 92 = 2 + 90. Another example is the decay of carbon-14 into nitrogen-14: In this case, the botto ...
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Nuclear Reactions and Their Applications

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Basic properties of atomic nuclei

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Physics 228 Today: April 22, 2012 Ch. 43 Nuclear

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Word - The Chemistry Book
Word - The Chemistry Book

... b. First to artificially transmute one element into another B. Nuclear reactions 1. Involve great quantities of energy Strong nuclear force overcomes electrostatic repulsion between protons 2. Differ from chemical reactions a. atomic numbers change b. some matter is changed to energy c. specific iso ...
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7.3 – Nuclear Reactions, Fission and Fusion 7.3.1 – Describe and

... Students must be familiar with the units MeV c -2 and GeV c -2 for mass 7.3.4 - Apply the Einstein mass – energy equivalence relationship 7.3.5 – Define the concepts of mass defect, binding energy and binding energy per nucleon 7.3.6 – Draw and annotate a graph showing the variation with nucleon num ...
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Chapter 30: Nuclear Physics What will we learn in this chapter?

... When Q > 0, the total mass decreases and we have an exoergic reaction; the kinetic energy increases. When Q < 0, the total mass increases and we have an endoergic reaction; the kinetic energy decreases. An endoergic reaction cannot occur unless the initial kinetic energy is at least as great as |Q|; ...
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APES-Chapter-3

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Chapter 7 Worksheet

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Nuclear fusion



In nuclear physics, nuclear fusion is a nuclear reaction in which two or more atomic nuclei come very close and then collide at a very high speed and join to form a new nucleus. During this process, matter is not conserved because some of the matter of the fusing nuclei is converted to photons (energy). Fusion is the process that powers active or ""main sequence"" stars.The fusion of two nuclei with lower masses than Iron-56 (which, along with Nickel-62, has the largest binding energy per nucleon) generally releases energy, while the fusion of nuclei heavier than iron absorbs energy. The opposite is true for the reverse process, nuclear fission. This means that fusion generally occurs for lighter elements only, and likewise, that fission normally occurs only for heavier elements. There are extreme astrophysical events that can lead to short periods of fusion with heavier nuclei. This is the process that gives rise to nucleosynthesis, the creation of the heavy elements during events such as supernova.Following the discovery of quantum tunneling by Friedrich Hund, in 1929 Robert Atkinson and Fritz Houtermans used the measured masses of light elements to predict that large amounts of energy could be released by fusing small nuclei. Building upon the nuclear transmutation experiments by Ernest Rutherford, carried out several years earlier, the laboratory fusion of hydrogen isotopes was first accomplished by Mark Oliphant in 1932. During the remainder of that decade the steps of the main cycle of nuclear fusion in stars were worked out by Hans Bethe. Research into fusion for military purposes began in the early 1940s as part of the Manhattan Project. Fusion was accomplished in 1951 with the Greenhouse Item nuclear test. Nuclear fusion on a large scale in an explosion was first carried out on November 1, 1952, in the Ivy Mike hydrogen bomb test.Research into developing controlled thermonuclear fusion for civil purposes also began in earnest in the 1950s, and it continues to this day. The present article is about the theory of fusion. For details of the quest for controlled fusion and its history, see the article Fusion power.
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