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The proton-proton chain reaction is one of two fusion reactions by which stars convert hydrogen to helium, the other being the CNO cycle. The proton-proton chain dominates in stars the size of the Sun or less.
To overcome the electromagnetic repulsion between two hydrogen nuclei requires a large amount of energy, and this reaction takes an average of 109 years to complete at the temperature of the Sun's core. Because of the slowness of this reaction the Sun is still shining; if it were faster, the Sun would have exhausted its hydrogen long ago.
In general, proton-proton fusion can occur only if the temperature (i.e. kinetic energy) of the protons is high enough that they can overcome the mutual Coulomb force repulsion. The theory that proton-proton reactions were 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 too low to overcome the Coulomb-force barrier. After the development of quantum mechanics, it was discovered that the tunneling of the wave functions of the protons through the repulsive barrier allowed for fusion at a lower temperature than the classical prediction.
The pp chain reaction
The first step involves the fusion of two hydrogen nuclei 1H (protons) into deuterium 2H, releasing a positron as one proton changes into a neutron, and a neutrino. with the neutrinos released in this step carrying energies up to 0.42 MeV.
This first step is extremely slow, because it depends on the weak interaction to convert one proton into a neutron. In fact this is the limiting step, with a proton waiting an average of 109 years before fusing into deuterium.
The positron immediately annihilates with one of the hydrogen's electrons, and their mass energy is carried off by two gamma ray photons.
- e+ + e− → 2γ + 1.02 MeV
After this the deuterium produced in the first stage can fuse with another hydrogen to produce a light isotope of helium, 3He:
- 2H + 1H → 3He + γ + 5.49 MeV
From here there are three posible paths to generate helium isotope 4He. In pp1 helium-4 comes from fusing two of the helium-3 nuclei produced; the pp2 and pp3 braches fuse 3He with a pre-existing 4He to make Beryllium-7. In the Sun, branch pp1 takes place with a frequency of 86%, pp2 with 14% and pp3 with 0.11%. There is also an extremely rare pp4 branch.
The pp I branch
- 3He +3He → 4He + 1H + 1H + 12.86 MeV
The pp II branch
| 3He + 4He | → | 7Be + γ | |
| 7Be + e− | → | 7Li + νe | |
| 7Li + 1H | → | 4He + 4He |
90% of the neutrinos produced in the reaction 7Be(e−,νe)7Li* carry an energy of 0.861 MeV, while the remaining 10% carry 0.383 MeV (depending on whether lithium-7 is excited or in the ground state).
The pp III branch
| 3He + 4He | → | 7Be + γ | |
| 7Be + 1H | → | 8B + γ | |
| 8B | → | 8Be + e+ + νe | |
| 8Be | ↔ | 4He + 4He |
The pp III chain is not a major source of energy in the Sun (only 0.11%), but was very important in the solar neutrino problem because it generates very high energy neutrinos (up to 14.06 MeV).
The pp IV or Hep
This reaction is predicted but has never been observed due to its great rarity (about 0.3 parts per million in the Sun). In this reaction, Helium-3 reacts directly with a proton to give helium-4, with an even higher possible neutrino energy (up to 18.8 MeV).- 3He + 1H → 4He + νe + e+
Energy release
Comparing the mass of the final helium-4 atom with the masses of the four protons reveals that 0.007 or 0.7% of the mass of the original protons has been lost. This mass has been converted into energy, in the form of gamma rays and neutrinos released during each of the individual reactions. The total energy we get in one whole chain is 26.73 MeV.Only energy released as gamma rays will interact with electrons and protons and heat the interior of the Sun. This heating supports the Sun and prevents it from collapsing under its own weight.
Neutrinos do not interact significantly with matter and do not help support the Sun against gravitational collapse. The neutrinos in the ppI, ppII and ppIII chains carry away the 2.0%, 4.0% and 28.3% of the energy respectively.Claus E. Rolfs, William S. Rodney: Cauldrons in the Cosmos, The University of Chicago Press, 1988, 354. pp
The pep reaction
Deuterium can also be produced by the rare pep (proton-electron-proton) reaction (electron capture):
- 1H + e− + 1H → 2H + νe
References
See also
Proton-Proton-Reaktion | Cadena protón-protón | Chaîne proton-proton | Catena protone-protone | 陽子-陽子連鎖反応 | 양성자-양성자 연쇄 반응 | Proton-proton ciklus | Proton-protoncyclus | Cykl protonowy
"Proton-proton chain reaction"