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In binding energy Nuclear binding energy is the energy required to separate an atomic nucleus completely into its constituent protons and neutrons, or, equivalently, the energy that would be liberated by combining individual protons and neutrons into a single nucleus. The hydrogen-2 nucleus, for example, composed of one. Nuclear binding energy. An example that illustrates nuclear binding energy is the nucleus of 12 C (carbon-12), which contains 6 protons and 6 neutrons. The protons are all positively charged and repel each other, but the nuclear force overcomes the repulsion and causes them to stick together. The nuclear force is a close-range force (it is. Nuclear binding energy curve. Source: hyperphysics.phy-astr.gsu.edu During the nuclear splitting or nuclear fusion, some of the mass of the nucleus gets converted into huge amounts of energy and thus this mass is removed from the total mass of the original particles, and the mass is missing in the resulting nucleus.
Nuclear Forces: There are fourknown types of field forces that we are aware of. We are already familiar with gravitational force and electromagnetic force. Since the nucleus of an atom is comprised of positivelycharged protons and neutrally charged neutrons, we might expect that the electromagnetic force between the protons would tend to blow the nucleus apart. But we also know that this does not routinelyhappen, so there must be another force acting in the nucleus to hold it together. The strong nuclear force is this force, named so because it is stronger than either the electromagnetic orgravitational forces. We don't know the nature of the strong nuclear force, but we do know that it is a short range force (on the order of 10-15 m) while gravity and the electromagneticforce act over long ranges. Thus, for very large nuclei, there is a potential for the electromagnetic force of the
protons to overcome the strong nuclear force and make the nucleus unstable. This manifests itself in a couple of ways. First, since the protons are the only nucleon that exert electromagnetic forceand neutrons and protons have strong nuclear forces holding them together, we find that atoms tend to have the same number of neutrons as protons up to the point where the atomic number is between 30and 40. Above that, the nucleus will have additional neutrons to hold it together. There is a point, however, when there cannot be enough neutrons added to overcome the em force, and the nuclidesbecome unstable. There are no completely stable nuclides above Lead (atomic number 82).
A fourth force, the weak nuclear force, manifests itself inradioactive decay. It is named the weak nuclear force because it is significantly weaker than the strong force. But of the four forces that act to bind a nucleus together, the very weakest is in factthe gravitational force.
Binding Energy is the energy that must be put into a nucleus in order tobreak it apart. The mass of a nucleus is always less than the mass of its individual protons and neutrons. The difference in mass has gone into some form of energy, such as kinetic energy orradiation. We call this difference mass defect. For example, we can find the Binding Energy of a helium nucleus (Helium 4). Helium weighs 4.002602 u. (We get this number from tables.) It iscomposed of 2 protons (mp = 1.007276 u) and 2 neutrons (mn = 1.008665 u). The 4 nucleons add to 4.032980 u. The difference, 0.030378 u has been converted to energy:
(0.030378 u)(931.5 MeV/u) =28.30 MeV.
This would be the amount of energy necessary to break up a Heliumnucleus.
Dirt devil dirt cup release button. The total binding energy is the energy of the constituent partsless the energy of the formed nucleus, as computed above. The average binding energy per nucleon is the total binding energy divided by the atomic mass number. For Helium, the averagebinding energy per nucleon is 28.30 MeV/4 = 7.1 MeV.
What Is Nuclear Binding Energy
For more on the topic, try:
A useful applet:http://lectureonline.cl.msu.edu/~mmp/kap30/Nuclear/nuc.htm
For Practice Problems, Try:Giancoli Multiple Choice PracticeQuestions(Don't worry if you can't solve all of them just yet!)
| The Curve of Binding Energy |
The key to energy production in stars lies in what nuclear physicists call the curve of binding energy, which is illustrated in the following figure.
| Curve of binding energy. |
This plot shows the amount of binding energy per nucleon (A nucleon is either aneutron or a proton. The nucleon number is the sum of the number ofneutrons plusprotons in a nucleus; thus, it is equal to the atomic mass number) as a function of the atomic mass number A. The energy unitsare MeV, which stands for 'million electron-volts', a standard unit of energy innuclear physics.
This curve indicates how stable atomic nuclei are; the higher the curve the morestable the nucleus. Notice the characteristic shape, with a peak near A=60. Thesenuclei (which are near iron in the periodic table and are calledthe iron peak nuclei) are the most stable in theUniverse. The shape of this curve suggests two possibilites for convertingsignificant amounts of mass into energy.Note that this is the 'upside down' version of the similar graph in text.There the vertical scale increases downward, here it increases upward.
Fission Reactions
From the curve of binding energy, the heaviest nuclei are less stable than thenuclei near A=60. This suggests that energy can be released if heavy nuclei splitapart into smaller nuclei having masses nearer A=60. This process is calledfission. It is the process that powers atomic bombs and nuclear powerreactors.Fusion Reactions
The curve of binding energy suggests a second way in which energy could be releasedin nuclear reactions. The lightest elements (like hydrogen and helium) have nucleithat are less stable than heavier elements up to A~60. Thus, sticking two lightnuclei together to form a heavier nucleus can release energy. This process iscalled fusion, and is the process that powers hydrogen (thermonuclear)bombs and (perhaps eventually) fusion energy reactors.In both fission and fusion reactions the total masses after the reaction areless than those before. The 'missing mass' appears as energy, with the amountgiven by the famous Einstein equation.
Stellar Energy Production
Nuclear Binding Energy Definition
Both fission and fusion reactions have the potential to convert a small amount ofmass into a large amount of energy and could conceivably account for the energysources of stars. However, stars are made from light elements (mostly hydrogen andhelium). Thus, fission cannot be initiated in stars as a source of energy, butfusion is quite possible if the right conditions prevail. As we shall see, theseconditions can be found in the cores of stars, and thermonuclear fusion is theprimary source of stellar energy.