There is almost universal agreement among astronomers that most of the mass in the Universe and most of the mass in
the Galactic halo is dark. Many lines of reasoning suggest that the dark matter consists of some new, as yet undiscovered,
weakly interacting massive particle (WIMP). There is now a vast experimental effort being surmounted to detect WIMPs
in the halo. The most promising techniques involve direct detection in low-background laboratory detectors and indirect
detection through observation of energetic neutrinos from annihilation of WIMPs that have accumulated in the Sun
and/or the Earth. Of the many WIMP candidates, perhaps the best motivated and certainly the most theoretically
developed is the neutralino, the lightest superpartner in many supersymmetric theories. We review the minimal
supersymmetric extension of the standard model and discuss prospects for detection of neutralino dark matter. We
review in detail how to calculate the cosmological abundance of the neutralino and the event rates for both direct- and
indirect-detection schemes, and we discuss astrophysical and laboratory constraints on supersymmetric models. We
isolate and clarify the uncertainties from particle physics, nuclear physics, and astrophysics that enter at each step in the
calculations. We briefly review other related dark-matter candidates and detection techniques.