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Neutrino-neutrino refraction dominates the flavor evolution in core-collapsesupernovae, neutron-star mergers, and the early universe. Ordinary neutrinoflavor conversion develops on timescales determined by the vacuum oscillationfrequency. However, when the neutrino density is large enough, collectiveflavor conversion may arise because of pairwise neutrino scattering. Pairwiseconversion is deemed to be fast as it is expected to occur on timescales thatdepend on the neutrino-neutrino interaction energy (i.e., on the neutrinonumber density) and is regulated by the angular distributions of electronneutrinos and antineutrinos. The enigmatic phenomenon of fast pairwiseconversion has been overlooked for a long time. However, because of the fastconversion rate, pairwise conversion may possibly occur in the proximity of theneutrino decoupling region with yet to be understood implications for thehydrodynamics of astrophysical sources and the synthesis of the heavy elements.We review the physics of this fascinating phenomenon and its implications forneutrino-dense sources.

New Developments in Flavor Evolution of a Dense Neutrino Gas