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The proton–proton chain, also commonly referred to as the Template:Nowrap chain, is one of two known sets of nuclear fusion reactions by which stars convert hydrogen to helium. It dominates in stars with masses less than or equal to that of the Sun,<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> whereas the CNO cycle, the other known reaction, is suggested by theoretical models to dominate in stars with masses greater than about 1.3 solar masses.<ref>Template:Cite book</ref>
In general, proton–proton fusion can occur only if the kinetic energy (temperature) of the protons is high enough to overcome their mutual electrostatic repulsion.<ref>Ishfaq Ahmad, The Nucleus, 1: 42, 59, (1971), The Proton type-nuclear fission reaction.</ref>
In the Sun, deuteron-producing events are rare. Diprotons are the much more common result of proton–proton reactions within the star, and diprotons almost immediately decay back into two protons. Since the conversion of hydrogen to helium is slow, the complete conversion of the hydrogen initially in the core of the Sun is calculated to take more than ten billion years.<ref>Kenneth S. Krane, Introductory Nuclear Physics, Wiley, 1987, p. 537.</ref>
Although sometimes called the "proton–proton chain reaction", it is not a chain reaction in the normal sense. In most nuclear reactions, a chain reaction designates a reaction that produces a product, such as neutrons given off during fission, that quickly induces another such reaction. The proton–proton chain is, like a decay chain, a series of reactions. The product of one reaction is the starting material of the next reaction. There are two main chains leading from hydrogen to helium in the Sun. One chain has five reactions, the other chain has six.
History of the theoryEdit
The theory that proton–proton reactions are the basic principle by which the Sun and other stars burn was advocated by Arthur Eddington in the 1920s. At the time, the temperature of the Sun was considered to be too low to overcome the Coulomb barrier. After the development of quantum mechanics, it was discovered that tunneling of the wavefunctions of the protons through the repulsive barrier allows for fusion at a lower temperature than the classical prediction.
In 1939, Hans Bethe attempted to calculate the rates of various reactions in stars. Starting with two protons combining to give a deuterium nucleus and a positron he found what we now call Branch II of the proton–proton chain. But he did not consider the reaction of two Template:Chem nuclei (Branch I) which we now know to be important.<ref>Template:Cite journal</ref> This was part of the body of work in stellar nucleosynthesis for which Bethe won the Nobel Prize in Physics in 1967.
The proton–proton chainEdit
The first step in all the branches is the fusion of two protons into a deuteron. As the protons fuse, one of them undergoes beta plus decay, converting into a neutron by emitting a positron and an electron neutrino<ref name=":0">Template:Cite book</ref> (though a small amount of deuterium nuclei is produced by the "pep" reaction, see below):
The positron will annihilate with an electron from the environment into two gamma rays. Including this annihilation and the energy of the neutrino, the net reaction
has a Q value (released energy) of 1.442 MeV:<ref name=":0" /> The relative amounts of energy going to the neutrino and to the other products is variable.
This is the rate-limiting reaction and is extremely slow due to it being initiated by the weak nuclear force. The average proton in the core of the Sun waits 9 billion years before it successfully fuses with another proton. It has not been possible to measure the cross-section of this reaction experimentally because it is so low<ref>Template:Cite book</ref> but it can be calculated from theory.<ref name= Adelberger/>
After it is formed, the deuteron produced in the first stage can fuse with another proton to produce the stable, light isotope of helium, Template:SimpleNuclide:
This process, mediated by the strong nuclear force rather than the weak force, is extremely fast by comparison to the first step. It is estimated that, under the conditions in the Sun's core, each newly created deuterium nucleus exists for only about one second before it is converted into helium-3.<ref name= Adelberger/>
In the Sun, each helium-3 nucleus produced in these reactions exists for only about 400 years before it is converted into helium-4.<ref>This time and the two other times above come from: Byrne, J. Neutrons, Nuclei, and Matter, Dover Publications, Mineola, NY, 2011, Template:ISBN, p 8.</ref> Once the helium-3 has been produced, there are four possible paths to generate Template:SimpleNuclide. In Template:Nowrap, helium-4 is produced by fusing two helium-3 nuclei; the Template:Nowrap and Template:Nowrap branches fuse Template:SimpleNuclide with pre-existing Template:SimpleNuclide to form beryllium-7, which undergoes further reactions to produce two helium-4 nuclei.
About 99% of the energy output of the sun comes from the various Template:Nowrap chains, with the other 1% coming from the CNO cycle. According to one model of the sun, 83.3 percent of the Template:SimpleNuclide produced by the various Template:Nowrap branches is produced via branch I while Template:Nowrap produces 16.68 percent and Template:Nowrap 0.02 percent.<ref name= Adelberger>Template:Cite journal See Figure 2. The caption is not very clear but it has been confirmed that the percentages refer to how much of each reaction takes place, or equivalently how much helium-4 is produced by each branch.</ref> Since half the neutrinos produced in branches II and III are produced in the first step (synthesis of a deuteron), only about 8.35 percent of neutrinos come from the later steps (see below), and about 91.65 percent are from deuteron synthesis. However, another solar model from around the same time gives only 7.14 percent of neutrinos from the later steps and 92.86 percent from the synthesis of deuterium nuclei.<ref>Template:Cite journal Calculated from model AGSS09 in Table 3.</ref> The difference is apparently due to slightly different assumptions about the composition and metallicity of the sun.
There is also the extremely rare Template:Nowrap branch. Other even rarer reactions may occur. The rate of these reactions is very low due to very small cross-sections, or because the number of reacting particles is so low that any reactions that might happen are statistically insignificant.
The overall reaction is:
releasing 26.73 MeV of energy, some of which is lost to the neutrinos.
The Template:Nowrap branchEdit
The complete chain releases a net energy of Template:Val<ref>Template:Cite book</ref> but 2.2 percent of this energy (0.59 MeV) is lost to the neutrinos that are produced.<ref>Template:Cite journal</ref> The Template:Nowrap branch is dominant at temperatures of 10 to Template:Val.<ref name=":1">Template:Cite book</ref> Below Template:Val, the Template:Nowrap chain proceeds at slow rate, resulting in a low production of Template:SimpleNuclide.<ref>Template:Cite journal</ref>
The Template:Nowrap branchEdit
The Template:Nowrap branch is dominant at temperatures of 18 to Template:Val.<ref name=":1" />
Note that the energies in the second reaction above are the energies of the neutrinos that are produced by the reaction. 90 percent of the neutrinos produced in the reaction of Template:SimpleNuclide to Template:SimpleNuclide carry an energy of Template:Val, while the remaining 10 percent carry Template:Val. The difference is whether the lithium-7 produced is in the ground state or an excited (metastable) state, respectively. The total energy released going from Template:Chem to stable Template:Chem is about 0.862 MeV, almost all of which is lost to the neutrino if the decay goes directly to the stable lithium.
The Template:Nowrap branchEdit
The last three stages of this chain, plus the positron annihilation, contribute a total of 18.209 MeV, though much of this is lost to the neutrino.
The Template:Nowrap chain is dominant if the temperature exceeds Template:Val.<ref name=":1" />
The Template:Nowrap chain is not a major source of energy in the Sun, but it was very important in the solar neutrino problem because it generates very high energy neutrinos (up to Template:Val).
The Template:Nowrap (Hep) branchEdit
This reaction is predicted theoretically, but it has never been observed due to its rarity (about Template:Val in the Sun). In this reaction, helium-3 captures a proton directly to give helium-4, with an even higher possible neutrino energy (up to Template:ValTemplate:Citation needed).
The mass–energy relationship gives Template:Val for the energy released by this reaction plus the ensuing annihilation, some of which is lost to the neutrino.
Energy releaseEdit
Comparing the mass of the final helium-4 nucleus with the masses of the four protons reveals that 0.7 percent of the mass of the original protons has been lost. This mass has been converted into energy, in the form of kinetic energy of produced particles, gamma rays, and neutrinos released during each of the individual reactions. The total energy yield of one whole chain is Template:Val.
Energy released as gamma rays will interact with electrons and protons and heat the interior of the Sun. Also kinetic energy of fusion products (e.g. of the two protons and the Template:Nuclide from the Template:Nowrap reaction) adds energy to the plasma in the Sun. This heating keeps the core of the Sun hot and prevents it from collapsing under its own weight as it would if the sun were to cool down.
Neutrinos do not interact significantly with matter and therefore do not heat the interior and thereby help support the Sun against gravitational collapse. Their energy is lost: the neutrinos in the Template:Nowrap, Template:Nowrap, and Template:Nowrap chains carry away 2.0%, 4.0%, and 28.3% of the energy in those reactions, respectively.<ref>Claus E. Rolfs and William S. Rodney, Cauldrons in the Cosmos, The University of Chicago Press, 1988, p. 354.</ref>
The following table calculates the amount of energy lost to neutrinos and the amount of "solar luminosity" coming from the three branches. "Luminosity" here means the amount of energy given off by the Sun as electromagnetic radiation rather than as neutrinos. The starting figures used are the ones mentioned higher in this article. The table concerns only the 99% of the power and neutrinos that come from the Template:Nowrap reactions, not the 1% coming from the CNO cycle.
| Branch | Percent of 4He produced |
Percent loss due to neutrino production |
Relative amount of energy lost |
Relative amount of luminosity produced |
Percentage of total luminosity |
|---|---|---|---|---|---|
| Branch I | Template:083.3% | Template:02% | 1.67% | 81.6% | Template:083.6% |
| Branch II | Template:016.68% | Template:04% | 0.67% | 16.0% | Template:016.4% |
| Branch III | Template:00.02% | 28.3% | 0.0057% | Template:00.014% | Template:00.015% |
| total | 100% | 2.34% | 97.7% | 100% |
The PEP reactionEdit
A deuteron can also be produced by the rare pep (proton–electron–proton) reaction (electron capture):
In the Sun, the frequency ratio of the pep reaction versus the Template:Nowrap reaction is 1:400. However, the neutrinos released by the pep reaction are far more energetic: while neutrinos produced in the first step of the Template:Nowrap reaction range in energy up to Template:Val, the pep reaction produces sharp-energy-line neutrinos of Template:Val. Detection of solar neutrinos from this reaction were reported by the Borexino collaboration in 2012.<ref>Template:Cite journal</ref>
Both the pep and Template:Nowrap reactions can be seen as two different Feynman representations of the same basic interaction, where the electron passes to the right side of the reaction as a positron. This is represented in the figure of proton–proton and electron-capture reactions in a star, available at the NDM'06 web site.<ref>Int'l Conference on Neutrino and Dark Matter, 7 Sept 2006, Session 14.</ref>
See alsoEdit
ReferencesEdit
External linksEdit
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