The Hot Dark Matter

Abstract

There is a puzzling contradiction: direct observations favor a low-mass-density universe ($0.2\le\Omega_m\le0.6$), but the only model which fits universe structure over more than three orders of magnitude in distance scale has a mix of hot (neutrino) and cold dark matter providing a critical density universe. Models of an open universe (low $\Omega_m$) or one adding a cosmological constant ($\Lambda$) to provide a critical energy density ($\Omega_m+ \Omega_\Lambda=1$) have probabilities of $<10^{-3}$. Two-neutrino dark matter works better than having the needed $\sim5$ eV of neutrino mass in one species of neutrino, and this is consistent with the only model which fits all present indications for neutrino mass: $\nu_\mu\to\nu_\tau$ accounting for the atmospheric anomaly (with $\nu_\mu$ and $\nu_\tau$ being the hot dark matter), $\bar\nu_\mu\to\bar\nu_e$ being observed by LSND, and $\nu_e\to\nu_s$ explaining the solar $\nu_e$ deficit. The LSND/KARMEN results are consistent with the needed mass of hot dark matter. Further support for this mass pattern is provided by the need for the sterile neutrino, $\nu_s$, to make possible heavy-element nucleosynthesis in supernovae. It is a fascinating question as to whether the hot dark matter paradox will be resolved by better measurements or by the introduction of new physics.