In cosmology, decoupling refers to a period in the development of the universe when different types of particles fall out of thermal equilibrium with each other. This occurs as a result of the expansion of the universe, as their interaction rates decrease up to this critical point. The two verified instances of decoupling since the Big Bang which are most often discussed are photon decoupling and neutrino decoupling, as these led to the cosmic microwave background and cosmic neutrino background, respectively. Photon decoupling is closely related to recombination, which occurred about 378,000 years after the Big Bang, when the universe was a hot opaqueplasma. During recombination, free electrons became bound to protons to form neutral hydrogen atoms. Because direct recombinations to the ground state of hydrogen are very inefficient, these hydrogen atoms generally form with the electrons in a high energy state, and the electrons quickly transition to their low energy state by emitting photons. Because the neutral hydrogen that formed was transparent to light, those photons which were not captured by other hydrogen atoms were able, for the first time in the history of the universe, to travel long distances. They can still be detected today, although they now appear as radio waves, and form the cosmic microwave background. They reveal crucial clues about how the universe formed.
Photon decoupling
Photon decoupling occurred during the epoch known as the recombination. During this time, electrons combined with protons to form hydrogen atoms, resulting in a sudden drop in free electrondensity. Decoupling occurred abruptly when the rate of Compton scattering of photons was approximately equal to the rate of expansion of the universe, or alternatively when the mean free path of the photons was approximately equal to the horizon size of the universe. After this photons were able to stream freely, producing the cosmic microwave background as we know it, and the universe became transparent. The interaction rate of the photons is given by where is the electron number density, is the electron cross sectional area, and is the speed of light. In the matter-dominated era, where is the cosmic scale factor. also decreases as a more complicated function of, at a faster rate than. By working out the precise dependence of and on the scale factor and equating, it is possible to show that photon decoupling occurred approximately 380,000 years after the Big Bang, at a redshift of when the universe was at a temperature around 3000 K.
Neutrino decoupling
Another example is the neutrino decoupling which occurred within one second of the Big Bang. Analogous to the decoupling of photons, neutrinos decoupled when the rate of weak interactions between neutrinos and other forms of matter dropped below the rate of expansion of the universe, which produced a cosmic neutrino background of freely streaming neutrinos. An important consequence of neutrino decoupling is that the temperature of this neutrino background is lower than the temperature of the cosmic microwave background.
Decoupling may also have occurred for the dark matter candidate, WIMPs. These are known as "cold relics", meaning they decoupled after they became non-relativistic. By calculating the hypothetical time and temperature of decoupling for non-relativistic WIMPs of a particular mass, it is possible to find their density. Comparing this to the measured density parameter of cold dark matter today of 0.222 0.0026 it is possible to rule out WIMPs of certain masses as reasonable dark matter candidates.
