
Dark matter core formation describes how dark matter clumps into dense nuclei.Dark matter core formation refers to the hypothesized process by which dark matter particles clump together into dense, compact structures, potentially forming 'dark nuclei' or dense cores within larger halos. This idea arises from models where dark matter has self-interactions or forms quantum condensates, leading to gravitational collapse on small scales. Such cores could influence the dynamics of galaxies, black hole formation, and the distribution of dark matter in the universe.
The concept gained traction in the 2000s, particularly with the development of self-interacting dark matter models by David Spergel and Paul Steinhardt (2000) and later studies of axion-like condensates.
In these models, dark matter particles interact with each other (beyond gravity) or behave as a quantum fluid, allowing them to lose energy and collapse into dense regions. For example, in self-interacting dark matter scenarios, collisions can cool the particles, causing them to sink toward the center of a halo and form a core. Alternatively, ultralight bosonic dark matter could form a Bose-Einstein condensate, producing a solitonic core with a characteristic density profile.
This research informs astrophysical observations of galaxy rotation curves and black hole mass distributions, helping to constrain the nature of dark matter.
Some models predict that dark matter cores could be so dense that they collapse into small black holes, potentially explaining the origin of intermediate-mass black holes.
| m_crit | variable | critical dark matter mass — mass kilogram |
| k_B | variable | Boltzmann constant — boltzmann constant joule per kelvin |
| T | variable | temperature — temperature kelvin |
| v | variable | velocity — velocity metre per second |










