Proton-proton chain

The proton-proton chain reaction (also known as the PP chain) is one of two fusion reactions by which stars convert hydrogen to helium, the other being the CNO cycle. The proton-proton chain is more important in stars the size of the Sun or less.

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. To overcome the electromagnetic repulsion between two hydrogen nuclei requires a large amount of energy, and this reaction takes an average of 10 billion years to complete. It is because of the slowness of this reaction that the Sun is still shining; if it where faster, the Sun would have exhausted its hydrogen long ago.

¹H + ¹H → ²H + e⁺ + ν_e + 0.42 MeV

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^- → 2&gamma + 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 + &gamma + 5.49 MeV

Finally, after millions of years, two of the helium nuclei ³He produced can fuse together to make the common helium isotope ⁴He, releasing two hydrogen nuclei to start the reaction again through three different paths called PP1, PP2 and PP3:

PP1:

³He +³He → ⁴He + ¹H + ¹H + 12.86 MeV

The complete PP1 chain reaction releases a net energy of 26.7 MeV. PP1 chain is dominant in temperatures of 10-14 million Kelvin. Below 10 million Kelvin, the PP chain does not produce much ⁴He.

PP2:

	3He + 4He	→	7Be + &gamma
	7Be + e-	→	7Li + νe
	7Li + 1H	→	4He + 4He

PP2 chain is dominant in temperatures of 14-23 million Kelvin.

PP3:

	3He + 4He	→	7Be + &gamma
	7Be + 1H	→	8B + γ
	8B	→	8Be + e+ + νe
	8Be	↔	4He + 4He

PP3 chain is dominant if the temperatures exceeds 23 million Kelvin.

See also:

• Triple-alpha process
• CNO cycle