
Magnetic fields originating from the early universe, influencing cosmic structure and dark matter.Primordial magnetic fields are magnetic fields that originated in the early universe, potentially before the formation of stars and galaxies. Unlike the magnetic fields we observe today in galaxies and clusters, which are often amplified by dynamo processes over billions of years, primordial fields could be relics of the very first instants after the Big Bang. They are of great interest because they may have influenced the formation of cosmic structure, seeding the density fluctuations that grew into galaxies, and could even be linked to the mysterious dark matter that pervades the cosmos.
The concept of primordial magnetic fields has been discussed since the mid-20th century, with early work by Ya. B. Zel'dovich and others in the 1960s-70s exploring their possible origins and cosmological consequences.
These fields would have been generated by processes in the early universe, such as phase transitions in the primordial plasma or during cosmic inflation. Once created, they would have been stretched and diluted by the expansion of the universe, but could still leave observable imprints. For example, they could affect the motion of charged particles in the intergalactic medium, subtly altering the cosmic microwave background radiation or the distribution of matter. Some theories suggest that primordial magnetic fields could interact with dark matter particles, providing a mechanism for dark matter to generate or amplify magnetic fields in galaxies, as hinted by recent research.
Studying primordial magnetic fields helps cosmologists probe the physics of the early universe and test models of cosmic inflation and particle physics beyond the Standard Model.
Some ancient bacteria on Earth produce chains of magnetic crystals, and their fossilized remains, called magnetofossils, can preserve records of the Earth's magnetic field history — a completely different kind of 'primordial' magnetism.
| \mathbf{B} | variable | Magnetic field vector — magnetic field tesla |
| t | variable | Time — time second |
| \mathbf{u} | variable | Velocity field of the conducting fluid — velocity metre per second |
| \eta | variable | Magnetic diffusivity — magnetic diffusivity square metre per second |
| \frac{\partial}{\par | operator | Partial derivative with respect to time — partial derivative |
| \nabla \times | operator | Curl operator — curl operator |
| \nabla^2 | operator | Laplacian operator — laplacian operator |
| P(k) | variable | power spectrum as function of wavenumber — power spectrum cubic metre |
| k | variable | wavenumber — wavenumber reciprocal metre |
| n | variable | spectral index — spectral index |
| ρ | variable | oscillation frequency parameter — oscillation frequency parameter |
| φ | variable | phase offset — phase radian |
| ln | operator | takes the natural logarithm of its argument — natural logarithm |
| sin | operator | computes the sine of the argument — sine function |












