A type of dark matter composed of scalar particles that interact weakly with gravity and other forces.Scalar dark matter is a class of dark matter candidates consisting of spin-zero particles that interact primarily through gravity and possibly weak additional forces. Unlike WIMPs (weakly interacting massive particles), scalar dark matter can be extremely light—with masses down to 10^-22 eV—forming a coherent wave-like state known as a Bose-Einstein condensate. This ultralight form, often called fuzzy dark matter, suppresses small-scale structure formation and could resolve discrepancies between cold dark matter simulations and observations of dwarf galaxies.
The idea of scalar fields as dark matter emerged in the 1990s, with the axion—a pseudoscalar particle—being the most studied example. The ultralight scalar dark matter scenario was popularized in the 2000s by Wayne Hu, Rennan Barkana, and Andrei Gruzinov.
Scalar particles obey the Klein-Gordon equation, and when their de Broglie wavelength is comparable to galactic scales, they behave as a quantum fluid rather than discrete particles. This fluid exerts a quantum pressure that prevents collapse below a certain scale, smoothing out density cusps in galaxy centers. The particles can also form solitonic cores—stable, oscillating lumps of dark matter—that mimic the observed flat rotation curves of dwarf galaxies.
Pulsar timing arrays and atomic interferometers are being used to search for the oscillating gravitational signatures of ultralight scalar dark matter, while black hole superradiance can extract energy from rotating black holes to create scalar clouds.
Scalar dark matter can form 'black hole bombs'—if a rotating black hole is surrounded by a scalar cloud, the cloud can extract rotational energy and grow exponentially, potentially producing gravitational waves detectable by LIGO.
| lambda_FS | variable | free streaming length — free streaming length metre |
| m_hm | variable | half-mode mass of dark matter — half mode mass kilogram |
| propto | operator | is proportional to — proportionality |
| S | variable | Action of the theory — action joule second |
| g | variable | Determinant of the spacetime metric tensor — metric determinant |
| φ | variable | Scalar field non-minimally coupled to gravity — scalar field |
| R | variable | Ricci scalar curvature — ricci scalar per metre squared |
| ∂φ | variable | Gradient of the scalar field — field gradient per metre |
| ∫ d⁴x | operator | Integration over four-dimensional spacetime — four dimensional integral |
| √(-g) | operator | Volume element factor for curved spacetime — sqrt negative metric determinant |
| (∂φ)² | operator | Kinetic term of the scalar field, contraction of its gradient with itself — kinetic term |
| r | variable | tensor-to-scalar ratio — dimensionless ratio |
| P_t | variable | power spectrum of tensor perturbations — power spectrum |
| P_s | variable | power spectrum of scalar perturbations — power spectrum |
| h | variable | scale height — length metre |
| T | variable | temperature — temperature kelvin |
| m | variable | mass of particle — mass kilogram |
| g | variable | gravitational acceleration — gravitational acceleration metre per second squared |
| k | constant | relates energy to temperature — boltzmann constant = 1.380649e-23 joule per kelvin |




