Encyclopedia
In
physics,
nuclear fusion is the process by which multiple
nuclei join together to form a heavier nucleus. It is accompanied by the release or absorption of
energy depending on the masses of the nuclei involved.
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.
Overview
Nuclear fusion of light elements releases the energy that causes
stars to shine and
hydrogen bombs to explode. Nuclear fusion of heavy elements occurs in the extremely high-energy conditions of
supernova explosions. Nuclear fusion in stars and supernovae is the primary process by which new natural elements are created. It is this reaction that is harnessed in
fusion power.
It takes considerable energy to force nuclei to fuse, even those of the least massive element,
hydrogen. But the fusion of lighter nuclei, which creates a heavier nucleus and a free neutron, will generally release more energy than it took to force them together—an
exothermic process that can produce self-sustaining reactions.
The
energy released in most
nuclear reactions is much larger than that for
chemical reactions, because the
binding energy that holds a nucleus together is far greater than the energy that holds
electrons to a nucleus. For example, the ionization energy gained by adding an electron to a hydrogen nucleus is 13.6 electron volts—less than one-millionth of the 17 MeV released in the D-T reaction shown to the top right.
Building upon the nuclear transmutation experiments of Ernest Rutherford done a few years earlier, fusion of light nuclei 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.
Requirements for fusion
A substantial energy barrier must be overcome before fusion can occur. At large distances two naked nuclei repel one another because of the repulsive
electrostatic force between their positively charged protons. If two nuclei can be brought close enough together, however, the electrostatic barrier can be overcome by the strong nuclear force which is stronger at close distances than the electrostatic repulsion.
When a nucleon such as a
proton or
neutron is added to a nucleus, the strong force attracts it to other nucleons, but primarily to its immediate neighbors due to the short range of the force. The nucleons in the interior of a nucleus have more neighboring nucleons than those on the surface. Since smaller nuclei have a larger surface-to-volume ratio, the binding energy per nucleon due to the strong force generally increases with the size of the nucleus but approaches a limiting value corresponding to that of a fully surrounded nucleon.
The electrostatic force, on the other hand, is an inverse-square force, so a proton added to a nucleus will feel an electrostatic repulsion from
all the other protons in the nucleus. The electrostatic energy per nucleon due to the electrostatic force thus increases without limit as nuclei get larger.
The net result of these opposing forces is that the binding energy per nucleon generally increases with increasing size, up to the elements
iron and
nickel, and then decreases for heavier nuclei. Eventually, the binding energy becomes negative and very heavy nuclei are not stable. The four most tightly bound nuclei, in decreasing order of binding energy, are
62Ni,
58Fe,
56Fe, and
60Ni . Even though the nickel isotope
62Ni is more stable, the iron isotope
56Fe is an order of magnitude more common. This is due to a greater disintegration rate for
62Ni in the interior of stars driven by photon absorption.
A notable exception to this general trend is the
helium-4 nucleus, whose binding energy is higher than that of
lithium, the next heavier element. The Pauli exclusion principle provides an explanation for this exceptional behavior - it says that because protons and neutrons are fermions, they cannot exist in exactly the same state. Each proton or neutron energy state in a nucleus can accommodate both a spin up particle and a spin down particle. Helium-4 has an anomalously large binding energy because its nucleus consists of two protons and two neutrons; so all four of its nucleons can be in the ground state. Any additional nucleons would have to go into higher energy states.
The situation is similar if two nuclei are brought together. As they approach each other, all the protons in one nucleus repel all the protons in the other. Not until the two nuclei actually come in contact can the strong nuclear force take over. Consequently, even when the final energy state is lower, there is a large energy barrier that must first be overcome. In chemistry, this would be known as
activation energy. In nuclear physics it is called the Coulomb barrier.
The Coulomb barrier is smallest for isotopes of hydrogen - they contain only a single positive charge in the nucleus. A bi-proton is not stable, so neutrons must also be involved, ideally in such a way that a helium nucleus, with its extremely tight binding, is one of the products.
Using deuterium-tritium fuel, the resulting energy barrier is about 0.1 MeV. In comparison, the energy needed to remove an
electron from hydrogen is 13.6 eV, about 7,500 times less energy. The result of the fusion is an unstable
5He nucleus, which immediately ejects a neutron with 14.1 MeV. The recoil energy of the remaining
4He nucleus is 3.5 MeV, so the total energy liberated is 17.6 MeV. This is many times more than what was needed to overcome the energy barrier.
If the energy to initiate the reaction comes from
accelerating one of the nuclei, the process is called
beam-target fusion; if both nuclei are accelerated, it is
beam-beam fusion. If the nuclei are part of a
plasma near thermal equilibrium, one speaks of
thermonuclear fusion. Temperature is a measure of the average kinetic energy of particles, so by heating the nuclei they will gain energy and eventually have enough to overcome this 0.1 MeV barrier. Converting the units between electronvolts and kelvins shows that the barrier would be overcome at a temperature in excess of 1
GK, obviously a very high temperature.
There are two effects that lower the actual temperature needed. One is the fact that temperature is the
average kinetic energy, implying that some nuclei at this temperature would actually have much higher energy than 0.1 MeV, while others would be much lower. It is the nuclei in the high-energy tail of the velocity distribution that account for most of the fusion reactions. The other effect is
quantum tunneling. The nuclei do not actually have to have enough energy to overcome the Coulomb barrier completely. If they have nearly enough energy, they can tunnel through the remaining barrier. For this reason fuel at lower temperatures will still undergo fusion events, at a lower rate.
The reaction
cross section s is a measure of the probability of a fusion reaction as a function of the relative velocity of the two reactant nuclei. If the reactants have a distribution of velocities, e.g. a thermal distribution with thermonuclear fusion, then it is useful to perform an average of over the distributions of the product of cross section and velocity. The reaction rate is
times the product of the reactant number densities:
If a species of nuclei is reacting with itself, such as the DD reaction, then the product must be replaced by .
increases from virtually zero at room temperatures up to meaningful magnitudes at temperatures of 10 - 100 keV. At these temperatures, well above typical ionization energies , the fusion reactants exist in a plasma state.
The significance of as a function of temperature in a device with a particular energy confinement time is found by considering the Lawson criterion.
Methods of fuel confinement
The fusion reaction can sustain itself if enough of the energy produced goes into keeping the fuel hot.
Gravitational confinement -
One force capable of confining the fuel well enough to satisfy the Lawson criterion is gravity. The mass needed, however, is so great that gravitational confinement is only found in stars. Even if the more reactive fuel deuterium were used, a mass greater than that of the planet Jupiter would be needed.
Magnetic confinement -
Since plasmas are very good electrical conductors, magnetic fields can also confine fusion fuel. A variety of magnetic configurations can be used, the most basic distinction being between mirror confinement and toroidal confinement, especially tokamaks and stellarators.
Inertial confinement -
A third confinement principle is to apply a rapid pulse of energy to a large part of the surface of a pellet of fusion fuel, causing it to simultaneously "implode" and heat to very high pressure and temperature. If the fuel is dense enough and hot enough, the fusion reaction rate will be high enough to burn a significant fraction of the fuel before it has dissipated. To achieve these extreme conditions, the initially cold fuel must be explosively compressed. Inertial confinement is used in the hydrogen bomb, where the driver is x-rays created by a fission bomb. Inertial confinement is also attempted in "controlled" nuclear fusion, where the driver is a laser, ion, or electron beam, or a Z-pinch.
Some other confinement principles have been investigated, such as muon-catalyzed fusion, the Farnsworth-Hirsch fusor , and bubble fusion.
Methods to produce fusion
A variety of methods are known to affect nuclear fusion. Some are "cold" in the strict sense that no part of the material is hot , some are "cold" in the limited sense that the bulk of the material is at a relatively low temperature and pressure but the reactants are not, and some are "hot" fusion methods that create macroscopic regions of very high temperature and pressure.
Locally cold fusion :
- Muon-catalyzed fusion is a well established and reproducible fusion process that occurs at ordinary temperatures. It was studied in detail by Steven Jones in the early 1980s. It has not been reported to produce net energy. Net energy production from this reaction is not believed to be possible because of the energy required to create muons, their 2.2 µs half-life, and the chance that a muon will bind to the new alpha particle and thus stop catalyzing fusion.
- low energy nuclear reaction is a controversial line of research to produce nuclear fusion
Generally cold, locally hot fusion :
- Accelerator based light-ion fusion. Using particle accelerators it is possible to achieve particle kinetic energies sufficient to induce many light ion fusion reactions. Of particular relevance into this discussion are devices referred to as sealed-tube neutron generators. These small devices are miniature particle accelerators filled with deuterium and tritium gas in an arrangement which allows ions of these nuclei to be accelerated against hydride targets, also containing deuterium and tritium, where fusion takes place. Hundreds of neutron generators are produced annually for use in the petroleum industry where they are used in measurement equipment for locating and mapping oil reserves. Despite periodic reports in the popular press by scientists claiming to have invented "table-top" fusion machines, neutron generators have been around for half a century. The sizes of these devices vary but the smallest instruments are often packaged in sizes smaller than a loaf of bread. These devices do not produce a net power output.
- In sonoluminescence, acoustic shock waves create temporary bubbles that collapse shortly after creation, producing very high temperatures and pressures. In 2002, Rusi P. Taleyarkhan reported the possibility that bubble fusion occurs in those collapsing bubbles . As of 2005, experiments to determine whether fusion is occurring give conflicting results. If fusion is occurring, it is because the local temperature and pressure are sufficiently high to produce hot fusion.
- The Farnsworth-Hirsch Fusor is a tabletop device in which fusion occurs. This fusion comes from high effective temperatures produced by electrostatic acceleration of ions. The device can be built inexpensively, but it too is unable to produce a net power output.
- Antimatter-initialized fusion uses small amounts of antimatter to trigger a tiny fusion explosion. This has been studied primarily in the context of making nuclear pulse propulsion feasible. This is not near becoming a practical power source, due to the cost of manufacturing antimatter alone.
- Pyroelectric fusion was reported in April 2005 by a team at UCLA. The scientists used a pyroelectric crystal heated from −34 to 7°C , combined with a tungsten needle to produce an electric field of about 25 gigavolts per meter to ionize and accelerate deuterium nuclei into an erbium deuteride target. Though the energy of the deuterium ions generated by the crystal has not been directly measured, the authors used 100 keV as an estimate in their modeling. At these energy levels, two deuterium nuclei can fuse together to produce a helium-3 nucleus, a 2.45 MeV neutron and bremsstrahlung. Although it makes a useful neutron generator, the apparatus is not intended for power generation since it requires far more energy than it produces.
Hot fusion :
The methods in the second group are examples of non-equilibrium systems, in which very high temperatures and pressures are produced in a relatively small region adjacent to material of much lower temperature. In his doctoral thesis for MIT, Todd Rider did a theoretical study of all non-equilibrium fusion systems. He demonstrated that all such systems will leak energy at a rapid rate due to bremsstrahlung, radiation produced when electrons in the plasma hit other electrons or ions at a cooler temperature and suddenly decelerate. The problem is not as pronounced in a hot plasma because the range of temperatures, and thus the magnitude of the deceleration, is much lower.
Important fusion reactions
Astrophysical reaction chains
The most important fusion process in nature is that which powers the stars. The net result is the fusion of four protons into one alpha particle, with the release of two positrons, two neutrinos , and energy, but several individual reactions are involved, depending on the mass of the star. For stars the size of the sun or smaller, the proton-proton chain dominates. In heavier stars, the CNO cycle is more important. Both types of processes are responsible for the creation of new elements as part of stellar nucleosynthesis.
At the temperatures and densities in stellar cores the rates of fusion reactions are still extremely slow. For example, at solar core temperature and density , the energy release rate is only ~0.1 microwatt/cm3 - millions of times less than the rate of energy release of ordinary candela and thousands of times less than the rate at which a human body generates heat. Thus, reproduction of stellar core conditions in a lab for nuclear fusion power production is completely impractical.
Criteria and candidates for terrestrial reactions
In man-made fusion, the primary fuel is not constrained to be protons and higher temperatures can be used, so reactions with larger cross-sections are chosen. This implies a lower Lawson criterion, and therefore less startup effort. Another concern is the production of neutrons, which activate the reactor structure radiologically, but also have the advantages of allowing volumetric extraction of the fusion energy and tritium breeding. Reactions that release no neutrons are referred to as aneutronic.
In order to be useful as a source of energy, a fusion reaction must satisfy several criteria. It must:
- be exothermic - This may be obvious, but it limits the reactants to the low Z side of the curve of binding energy. It also makes helium He-4 the most common product because of its extraordinarily tight binding, although He3 and H3 also show up
- involve low Z nuclei - This is because the electrostatic repulsion must be overcome before the nuclei are close enough to fuse
- have two reactants - At anything less than stellar densities, three body collisions are too improbable. It should be noted that in inertial confinement, both stellar densities and temperatures are exceeded to compensate for the shortcomings of the third parameter of the Lawson criterion, ICF's very short confinement time.
- have two or more products - This allows simultaneous conservation of energy and momentum without relying on the electromagnetic force
- conserve both protons and neutrons - The cross sections for the weak interaction are too small
Few reactions meet these criteria. The following are those with the largest cross sections:
| width="50px" | D | T | ? | | 4He | | + | | n | | |
>D | D | ? | | T | | + | | p | | | | | | 50% | > | | | ? | | 3He | | + | | n | | | | | | 50% | >D | 3He | ? | | 4He | | + | | p | | >T | T | ? | | 4He | | + | 2 | n | 11.3 MeV>3He | 3He | ? | | 4He | | + | 2 | p | 12.9 MeV>3He | T | ? | | 4He | | + | | p | | + | n | 12.1 MeV | 51% | > | | | ? | | 4He | | + | | D | | | | | | 43% | > | | | ? | | 4He | | + | | n | | + | p | | | 6% | >D | 6Li | ? | 2 | 4He | 22.4 MeV>p | 6Li | ? | | 4He | | + | | 3He | | >3He | 6Li | ? | 2 | 4He | | + | | p | 16.9 MeV>p | 11B | ? | 3 | 4He | 8.7 MeV
p , D , and T are shorthand notation for the main three isotopes of hydrogen.
For reactions with two products, the energy is divided between them in inverse proportion to their masses, as shown. In most reactions with three products, the distribution of energy varies. For reactions that can result in more than one set of products, the branching ratios are given.
Some reaction candidates can be eliminated at once. The D-6Li reaction has no advantage compared to p-11B because it is roughly as difficult to burn but produces substantially more neutrons through D-D side reactions. There is also a p-7Li reaction, but the cross section is far too low except possible for Ti > 1 MeV, but at such high temperatures an endothermic, direct neutron-producing reaction also becomes very significant. Finally there is also a p-9Be reaction, which is not only difficult to burn, but 9Be can be easily induced to split into two alphas and a neutron.
In addition to the fusion reactions, the following reactions with neutrons are important in order to "breed" tritium in "dry" fusion bombs and some proposed fusion reactors:
- n + 6Li ? T + 4He
- n + 7Li ? T + 4He + n
To evaluate the usefulness of these reactions, in addition to the reactants, the products, and the energy released, one needs to know something about the cross section. Any given fusion device will have a maximum plasma pressure that it can sustain, and an economical device will always operate near this maximum. Given this pressure, the largest fusion output is obtained when the temperature is chosen so that /T˛ is a maximum. This is also the temperature at which the value of the triple product nTt required for ignition is a minimum. This optimum temperature and the value of /T˛ at that temperature is given for a few of these reactions in the following table.
| fuel | T [keV] | /T˛ [mł/s/keV˛] |
|---|
| D-T | 13.6 | |
| D-D | 15 | |
| D-3He | 58 | |
| p-6Li | 66 | |
| p-11B | 123 | |
Note that many of the reactions form chains. For instance, a reactor fueled with T and 3He will create some D, which is then possible to use in the D + 3He reaction if the energies are "right". An elegant idea is to combine the reactions and . The 3He from reaction can react with 6Li in reaction before completely thermalizing. This produces an energetic proton which in turn undergoes reaction before thermalizing. A detailed analysis shows that this idea will not really work well, but it is a good example of a case where the usual assumption of a Maxwellian plasma is not appropriate.
Neutronicity, confinement requirement, and power density
Any of the reactions above can in principle be the basis of fusion power production. In addition to the temperature and cross section discussed above, we must consider the total energy of the fusion products Efus, the energy of the charged fusion products Ech, and the atomic number Z of the non-hydrogenic reactant.
Specification of the D-D reaction entails some difficulties, though. To begin with, one must average over the two branches and . More difficult is to decide how to treat the T and 3He products. T burns so well in a deuterium plasma that it is almost impossible to extract from the plasma. The D-3He reaction is optimized at a much higher temperature, so the burnup at the optimum D-D temperature may be low, so it seems reasonable to assume the T but not the 3He gets burned up and adds its energy to the net reaction. Thus we will count the DD fusion energy as Efus = /2 = 12.5 MeV and the energy in charged particles as Ech = /2 = 4.2 MeV.
Another unique aspect of the D-D reaction is that there is only one reactant, which must be taken into account when calculating the reaction rate.
With this choice, we tabulate parameters for four of the most important reactions.
| fuel | Z | Efus [MeV] | Ech [MeV] | neutronicity |
|---|
| D-T | 1 | 17.6 | 3.5 | 0.80 |
| D-D | 1 | 12.5 | 4.2 | 0.66 |
| D-3He | 2 | 18.3 | 18.3 | ~0.05 |
| p-11B | 5 | 8.7 | 8.7 | ~0.001 |
The last column is the neutronicity of the reaction, the fraction of the fusion energy released as neutrons. This is an important indicator of the magnitude of the problems associated with neutrons like radiation damage, biological shielding, remote handling, and safety. For the first two reactions it is calculated as /Efus. For the last two reactions, where this calculation would give zero, the values quoted are rough estimates based on side reactions that produce neutrons in a plasma in thermal equilibrium.
Of course, the reactants should also be mixed in the optimal proportions. This is the case when each reactant ion plus its associated electrons accounts for half the pressure. Assuming that the total pressure is fixed, this means that density of the non-hydrogenic ion is smaller than that of the hydrogenic ion by a factor 2/. Therefore the rate for these reactions is reduced by the same factor, on top of any differences in the values of /T˛. On the other hand, because the D-D reaction has only one reactant, the rate is twice as high as if the fuel were divided between two hydrogenic species.
Thus there is a "penalty" of for non-hydrogenic fuels arising from the fact that they require more electrons, which take up pressure without participating in the fusion reaction. There is at the same time a "bonus" of a factor 2 for D-D due to the fact that each ion can react with any of the other ions, not just a fraction of them.
We can now compare these reactions in the following table.
| fuel | /T˛ | penalty/bonus | reactivity | Lawson criterion | power density |
|---|
| D-T | | 1 | 1 | 1 | 1 |
| D-D | | 2 | 48 | 30 | 68 |
| D-3He | | 2/3 | 83 | 16 | 80 |
| p-11B | | 1/3 | 1240 | 500 | 2500 |
The maximum value of /T˛ is taken from a previous table. The "penalty/bonus" factor is that related to a non-hydrogenic reactant or a single-species reaction. The values in the column "reactivity" are found by dividing 1.24 by the product of the second and third columns. It indicates the factor by which the other reactions occur more slowly than the D-T reaction under comparable conditions. The column "Lawson criterion" weights these results with Ech and gives an indication of how much more difficult it is to achieve ignition with these reactions, relative to the difficulty for the D-T reaction. The last column is labeled "power density" and weights the practical reactivity with Efus. It indicates how much lower the fusion power density of the other reactions is compared to the D-T reaction and can be considered a measure of the economic potential.
Bremsstrahlung losses
The ions undergoing fusion will essentially never occur alone but will be mixed with electrons that neutralize the ions' electrical charge and form a plasma. The electrons will generally have a temperature comparable to or greater than that of the ions, so they will collide with the ions and emit Bremsstrahlung. The Sun and stars are opaque to Bremsstrahlung, but essentially any terrestrial fusion reactor will be optically thin at relevant wavelengths. Bremsstrahlung is also difficult to reflect and difficult to convert directly to electricity, so the ratio of fusion power produced to Bremsstrahlung radiation lost is an important figure of merit. This ratio is generally maximized at a much higher temperature than that which maximizes the power density . The following table shows the rough optimum temperature and the power ratio at that temperature for several reactions.
| fuel | Ti | Pfusion/PBremsstrahlung |
|---|
| D-T | 50 | 140 |
| D-D | 500 | 2.9 |
| D-3He | 100 | 5.3 |
| 3He-3He | 1000 | 0.72 |
| p-6Li | 800 | 0.21 |
| p-11B | 300 | 0.57 |
The actual ratios of fusion to Bremsstrahlung power will likely be significantly lower for several reasons. For one, the calculation assumes that the energy of the fusion products is transmitted completely to the fuel ions, which then lose energy to the electrons by collisions, which in turn lose energy by Bremsstrahlung. However because the fusion products move much faster than the fuel ions, they will give up a significant fraction of their energy directly to the electrons. Secondly, the plasma is assumed to be composed purely of fuel ions. In practice, there will be a significant proportion of impurity ions, which will lower the ratio. In particular, the fusion products themselves must remain in the plasma until they have given up their energy, and will remain some time after that in any proposed confinement scheme. Finally, all channels of energy loss other than Bremsstrahlung have been neglected. The last two factors are related. On theoretical and experimental grounds, particle and energy confinement seem to be closely related. In a confinement scheme that does a good job of retaining energy, fusion products will build up. If the fusion products are efficiently ejected, then energy confinement will be poor, too.
The temperatures maximizing the fusion power compared to the Bremsstrahlung are in every case higher than the temperature that maximizes the power density and minimizes the required value of the fusion triple product. This will not change the optimum operating point for D-T very much because the Bremsstrahlung fraction is low, but it will push the other fuels into regimes where the power density relative to D-T is even lower and the required confinement even more difficult to achieve. For D-D and D-3He, Bremsstrahlung losses will be a serious, possibly prohibitive problem. For 3He-3He, p-6Li and p-11B the Bremsstrahlung losses appear to make a fusion reactor using these fuels impossible. Some ways out of this dilemma are considered — and rejected — in .
See also
...
...
- ITER – Experimental fusion reactor under construction in France
- Periodic table
External links
- – A guide to fusion from the UKAEA
- A Washington, DC area lobbying organization; "a non-profit, tax-exempt research and educational foundation, providing timely information on the status of fusion development." Edits the Journal of Fusion Energy.
- – Belgian Nuclear Research Centre
- – Nuclear Fusion Research at the Joint European Taurus
- What is Nuclear Fusion?
-
-
-
-
- First chapter of The Physics of Inertial Fusion, Stefano Atzeni and Jürgen Meyer-ter-Vehn
