Dark matter composed of fermions, particles with half-integer spin, as opposed to bosonic candidates.Fermionic dark matter is a class of dark matter candidates composed of fermions, particles with half-integer spin such as electrons, protons, or hypothetical particles like sterile neutrinos. Unlike bosonic dark matter (e.g., axions), fermions obey the Pauli exclusion principle, which prevents two identical fermions from occupying the same quantum state. This property has profound implications for the structure and dynamics of dark matter halos, particularly at high densities.
The idea that dark matter could be fermionic dates back to the 1980s, with sterile neutrinos proposed as a specific candidate in 1994 by Dodelson and Widrow. The concept gained traction in the 2000s as a way to address small-scale structure problems in cold dark matter simulations.
Because fermions cannot be compressed indefinitely, they exert a degeneracy pressure that counteracts gravitational collapse. This sets a maximum density for a fermionic dark matter halo, known as the Chandrasekhar limit (for a given mass). For light fermions (e.g., a few keV), this pressure can prevent the formation of cusps in galaxy centers, potentially explaining observed flat rotation curves. For heavier fermions, the pressure is negligible on galactic scales, and they behave like cold dark matter.
It is used in astrophysical models to explain the rotation curves of dwarf galaxies and to predict the mass of dark matter particles from observations of galaxy clusters.
If dark matter is a fermion with a mass of a few keV, it would form a 'degenerate Fermi ball' in the center of galaxies, which could be as dense as a neutron star but invisible.










