Three-neutrino mixing schemes suggested by Cardall & Fuller and Acker & Pakvasa are compared and contrasted. Both of these schemes seek to solve the solar and atmospheric neutrino problems and to account for the possible neutrino oscillation signal in the LSND experiment. These neutrino oscillation schemes have different atmospheric and solar neutrino signatures that will be discriminated by Super-Kamiokande and SNO. They will also have different signatures in proposed long-baseline accelerator and reactor experiments. In particular, both of these schemes would give dramatic (and dramatically different) signals in an "intermediate baseline" experiment, such as the proposed ICARUS detector in the Jura mountains 17 km from CERN. © 1997 Elsevier Science B.V.

We suggest a new method for detection of neutrino bursts generated by distant supernovas in our galaxy and in the local group of galaxies. This new method is based on the detection of neutrons produced in the inelastic scattering of νμ and ντ neutrinos with nuclei via the neutral current channel. The advantages of such a detector are (1) the enhancement of neutrino scattering cross sections due to nuclear collective effects, (2) the selective detection of νμ and ντ supernova neutrinos, and (3) the existence of large geological deposits of suitable neutrino detector materials in nature. © 1990.

We propose the construction of a compact Muon Collider Higgs Factory. Such a machine can produce up to \sim 14,000 at 8\times 10^{31} cm^-2 sec^-1 clean Higgs events per year, enabling the most precise possible measurement of the mass, width and Higgs-Yukawa coupling constants.

We propose the construction of, and describe in detail, a compact Muon Collider s-channel Higgs Factory.