A topic in the Open Knowledge Graph — a free, open map of 15,290 topics and the order to learn them in.
Astrophysical and cosmological observations establish that approximately 27% of the universe's energy density consists of non-baryonic dark matter that interacts gravitationally but has not been detected electromagnetically. Particle physics provides several well-motivated candidates: weakly interacting massive particles (WIMPs), axions, sterile neutrinos, and others. Each candidate has distinct production mechanisms, mass ranges, and experimental signatures, driving a diverse program of direct detection, indirect detection, and collider searches.
The evidence for dark matter comes from multiple independent observations spanning scales from individual galaxies to the observable universe. Galaxy rotation curves, gravitational lensing, the dynamics of galaxy clusters, the cosmic microwave background power spectrum, and the large-scale structure of the universe all require a non-baryonic matter component that constitutes about 27% of the total energy density. The properties of dark matter are constrained: it must be non-relativistic at the time of structure formation (cold), long-lived (stable on cosmological timescales), and interact weakly (if at all) with photons and baryons.
WIMPs have been the leading dark matter candidate for decades, motivated by the hierarchy problem (new particles at the weak scale) and the WIMP miracle (thermal freeze-out naturally producing the right relic density). SUSY neutralinos, Kaluza-Klein photons, and other BSM particles at the 100 GeV - 1 TeV scale are specific WIMP candidates. The experimental program has three prongs: (1) direct detection (measuring WIMP-nucleus scattering in underground detectors), (2) indirect detection (searching for WIMP annihilation products in the galaxy -- gamma rays, antiprotons, positrons, neutrinos), and (3) collider production (producing dark matter at the LHC, detected as missing transverse energy). Despite decades of effort, no confirmed detection has occurred, and the remaining WIMP parameter space is shrinking.
The QCD axion is motivated independently by the strong CP problem: why the QCD vacuum angle theta is observed to be less than ~10-10, despite having no reason within the Standard Model to be small. The Peccei-Quinn mechanism dynamically relaxes theta to zero by introducing a new global U(1) symmetry, and the axion is the pseudo-Goldstone boson of this symmetry. The axion mass and couplings are inversely related to the symmetry-breaking scale f_a: m_a ~ 6 x 10-6 eV * (1012 GeV / f_a). The allowed window for the axion dark matter mass is roughly 10-6 to 10-3 eV (with model-dependent boundaries), and experiments are beginning to probe this range.
Beyond WIMPs and axions, a rich landscape of dark matter candidates exists: sterile neutrinos (keV-scale, produced through mixing with active neutrinos, warm dark matter), dark photons (new U(1) gauge bosons kinetically mixed with the photon), asymmetric dark matter (where the dark matter abundance is set by a matter-antimatter asymmetry analogous to baryons), primordial black holes, and fuzzy dark matter (ultra-light axion-like particles with m ~ 10-22 eV whose de Broglie wavelength is on galactic scales). The breadth of candidates reflects our ignorance of the dark sector and motivates a diverse experimental program spanning underground laboratories, space-based observatories, microwave cavities, atom interferometers, and colliders.
No topics depend on this one yet.