[en] The history and recent progress of atmospheric neutrinos are reviewed. An emphasis is placed on results from experiments other than Super-Kamiokande

[en] MINOS is the first large magnetic detector deep underground and is the first to measure the muon charge ratio with high statistics in the region near 1 TeV.[1] An approximate formula for the muon charge ratio can be expressed in terms of η_π = 115 GeV, η_K = 850 GeV and E_μ^surfaceThe implications for K production in the atmosphere will be discussed

[en] Following incredible recent progress in understanding neutrino oscillations, many new ambitious experiments are being planned to study neutrino properties. The most important may be to find a non-zero value of θ₁₃. The most promising way to do this appears to be to measure ν_μ -> ν_e oscillations with an E/L near Δm²_atmo. Future neutrino experiments are great. (author)

[en] Current and future neutrino oscillation experiments are discussed with an emphasis on those that will measure or further limit the neutrino oscillation parameter θ₁₃. Some ν_e disappearance experiments are being planned at nuclear reactors, and more ambitious ν_μ→ν_e appearance experiments are being planned using accelerator beams.

[en] The Soudan 2 collaboration has measured the atmospheric neutrino flavor ratio with 2.63 kiloton years of exposure. Our measured flavor ratio is 0.67±0.15(stat)+0.04-0.06(syst). The neutrino induced horizontal muon flux has been measured to be Φ_μ=(4.12±1.1±0.58)x10^-13cm^-2sr^-1s^-1

[en] Fermilab is embarking upon a neutrino oscillation program which includes a long-baseline neutrino experiment MINOS. MINOS will be a 10 kiloton detector located 730 km Northwest of Fermilab in the Soudan underground laboratory. It will be sensitive to neutrino oscillations with parameters above Δm²∼3x10^-3eV² and sin²(2θ)∼0.02

[en] This contribution to the proceedings of the 2008 NOW Workshop summarizes current and future long-baseline neutrino oscillation experiments in the United States.

[en] The Deep Underground Neutrino Experiment (DUNE) is a worldwide effort to construct a next-generation long-baseline neutrino experiment based at the Fermi National Accelerator Laboratory. It is a merger of previous efforts and other interested parties to build, operate, and exploit a staged 40 kt liquid argon detector at the Sanford Underground Research Facility 1300 km from Fermilab, and a high precision near detector, exposed to a 1.2 MW, tunable ν beam produced by the PIP-II upgrade by 2024, evolving to a power of 2.3 MW by 2030. The neutrino oscillation physics goals and the status of the collaboration and project are summarized in this paper.

[en] We describe the status of our effort to realize a first neutrino factory and the progress made in understanding the problems associated with the collection and cooling of muons towards that end. We summarize the physics that can be done with neutrino factories as well as with intense cold beams of muons. The physics potential of muon colliders is reviewed, both as Higgs Factories and compact high energy lepton colliders. The status and timescale of our research and development effort is reviewed as well as the latest designs in cooling channels including the promise of ring coolers in achieving longitudinal and transverse cooling simultaneously. We detail the efforts being made to mount an international cooling experiment to demonstrate the ionization cooling of muons

[en] Neutrinos play an exceptional role in particle or nuclear physics as well as in astrophysics. Postulated by Pauli in 1930, they were named by Fermi in 1933 and experimentally discovered by Reines and Cowan in 1956. A second family of neutrinos was discovered in 1962 and a third in 1975. The CERN collider LEP proved in 1989 that 3 types of interacting neutrinos are enough in the standard model of particle physics. They are named electron-neutrino (ν_e), muon-neutrino (ν_μ) and tau-neutrino (ν_τ), associated to the charged leptons electron, muon and tau. They have no charge, a very tiny mass and interact only weakly, so these elusive particles can cross large quantity of matter (like the Sun or the Earth) without interacting. Emitted in huge numbers (about 1020 per second) in nuclear reactors, they are also artificially produced in man-made accelerators which deliver intense neutrino beams. But the main source of neutrinos is the Universe itself: the relic neutrinos from the Big Bang have been wandering for more than 13.6 billion years, with a density of 330 per cm³ everywhere. Starting with the fusion of two protons, nuclear reactions in the core of the Sun produce about 2 10³⁸ electron-neutrinos per second, which means 65 billions of neutrinos per second per cm² on Earth. Supernova explosions emit about 10⁵⁸ neutrinos in a few seconds and the central engines of active galactic nuclei produce them abundantly. On Earth, many neutrinos are produced by the interaction of high energy cosmic rays in the upper atmosphere and are also emitted by radioactive elements in the crust and the mantle of the Earth. We are bathed in neutrinos which cross us continually and abundantly. Witnesses of the core of the Sun, solar electron-neutrinos have been observed since 1968, but their number is significantly less than what is predicted by solar models built by astrophysicists. It took more than 30 years to solve the problem of the deficit, when the SNO experiment showed in 2001 that part of the solar electron-neutrinos had been transformed into mu-neutrinos or tau-neutrinos. This was explained by the fact that neutrinos were oscillating between the three families, a mechanism invented by Pontecorvo in 1958 and authorized by quantum mechanics (mechanism completed by the MSW effect for solar neutrinos). In fact the oscillation mechanism was first observed in 1998 by the SuperKamiokande experiment via the study of atmospheric neutrinos: muon-neutrinos produced in the atmosphere at the antipodes were oscillating into tau-neutrinos during their travel through the Earth. Neutrino oscillation is possible only if neutrinos have a mass (which is not necessary in the minimal standard model of particle physics) and its discovery opens the door towards, at least, the completion of the standard model. Since 1970, neutrino beams have been used also to study neutrino properties but also to penetrate deep inside the nucleons and unveil their fine structure. This document is the compilation of all presentations given at the conference