General overviews:

Estaban Roulet, Neutrino in physics and astrophysics hep-ph/9910383

W.C. Haxton and B.R.Holstein, Neutrino Physics, hep-ph/9905257

Proposed subjects:

Neutrinos from GRB (Jan Conrad)

E.Waxman and J.Bachcall, Neutrinos from GRB: 1018 eV, hep-ph/9909286

We show that a significant fraction of the energy of a gamma-ray burst(GRB) is probably converted to a burst of 10^{17}-10^{19} eV neutrinos and multiple GeV gammas that follow the GRB by > 10 s . If, as previously suggested, GRB's accelerate protons to ~10^{20} eV, then both the neutrinos and the gammas may be detectable.

F.Halzen and D.W Hooper, Neutrino evenr rates from GRB,hep-ph/9908138

We recalculate the diffuse flux of high energy neutrinos produced by Gamma Ray Bursts (GRB) in the relativistic fireball model. Although we confirm that the average single burst produces only ~10^{-2} high energy neutrino events in a detector with 1 km^2 effective area, i.e. about 10 events per year, we show that the observed rate is dominated by burst-to-burst fluctuations which are very large. We find event rates that are expected to be larger by one order of magnitude, likely more, which are dominated by a few very bright bursts. This greatly simplifies their detection.

Arnon Dar, High Energy Cosmic Rays, Gamma rays And Neutrino From Jetted GRBS, astro-ph/9905315

Recent observations suggest that gamma ray bursts (GRBs) and their afterglows are produced in star formation regions in distant galaxies by highly relativistic jets that happen to point in our direction. Relativistic beaming collimates the emission from the highlyrelativistic jets into small solid angles along the jet direction. It implies that we are seeing only a small fraction of the events that produce GRBs. The observed GRB rate then requires an event rate which is comparable to the birth rate of neutron stars (NS). The highly relativistic jets sweep up ambient matter along their trajectories, accelerate it to cosmic ray (CR) energies and disperse it in hot

spots which they form when they stop in the galactic halo. With an event rate comparable to the NS birth rate, such events in our Galaxy may be the main source of Galactic cosmic rays at all energies. Internal interactions and/or external interactions of these jets with high column density matter and/or radiation at their production sites or along their trajectories can produce high energy gamma rays and neutrinos that are highly beamed along the jet direction. Jetted GRBs, like blazars, may be much more fluent in high energygamma rays and neutrinos than in MeV gamma rays. But, TeV gamma rays from large cosmological distances are unobservable

because of their attenuation by electron-positron pair creation on the intergalactic infrared background radiation. However, high energy neutrinos from distant GRBs may be observed with large surface/volume telescopes which are under construction. TeV gamma rays and high energy neutrinos may also be detected from relatively nearby GRBs by the existing moderate size detectors, but with a much smaller rate.

Cosmic Neutrinos (?)

C.Hagmann, Cosmic Neutrinos and their Detection, astro-ph/9905258

The standard Big-Bang theory predicts a cosmic neutrino background with an average number density of $\sim 100/cm^3$ per flavor. The most promising way of its detection is measuring the feeble ``neutrino wind'' forces exerted on macroscopic targets. The expected acceleration is $\sim 10^{-23} cm/s^2$ for Dirac neutrinos with a local number density $\sim 10^7/cm^3$. A novel torsion balance design is presented, which addresses the sensitivity-limiting factors of existing balances, such as seismic and thermal noise, and angular readout resolution and stability.

Long baseline neutrino oscillation to tau-neutrinos (Julio Rodriques)

John G. Learned and Sandip Pakvasa Detecting Tau Neutrino Oscillations at PeV Energies, hep-ph/9408296

It is suggested that a large deep underocean (or ice) neutrino detector, given the presence of significant numbers of neutrinos in the PeV energy range as predicted by various models of Active Galactic Nuclei, can make unique measurements of the properties of neutrinos. It will be possible to observe the existence of the tau neutrino, measure its mixing with other flavors, in fact test themixing pattern for all three flavors based upon the mixing parameters suggested by the atmospheric and solar neutrino data, andmeasure the tau neutrino cross section. The key signature is the charged current tau neutrino interaction, which produces a double cascade, one at either end of a lightly radiating track. At a few PeV these cascades would be separated by roughly 100 m, and thus be easily resolvable in next generation DUMAND-like detectors. First examples might be found in detectors presently under construction. Future applications are precise neutrino astronomy and earth tomography. This paper is an expanded version of

hep-ph/9405296, for publication.

S.Iyver and M.Hall, Searching for $\nu_\mu \to \nu_\tau$ Oscillations with Extragalactic Neutrinos, hep-ph/9909393

We propose a novel approach for studying $\nu_\mu \to \nu_\tau$ oscillations with extragalactic neutrinos. Active Galactic Nuclei and Gamma Ray Bursts are believed to be sources of ultrahigh energy muon neutrinos. With distances of 100 Mpc or more, theyprovide an unusually long baseline for possible detection of $\nu_\mu \to \nu_\tau$ with mixing parameters $\Delta m^2$ down to $10^{-17}$eV$^2$, many orders of magnitude below the current accelerator experiments. By solving the coupled transport equations, we show that high-energy $\nu_\tau$'s, as they propagate through the earth, cascade down in energy, producing the

enhancement of the incoming $\nu_\tau$ flux in the low energy region, in contrast to the high-energy $\nu_\mu$'s, which get absorbed. For an AGN quasar model we find the $\nu_\tau$ flux to be a factor of 2 to 2.5 larger than the incoming flux in the energy range between $10^2$ GeV and $10^4$ GeV, while for a GRB fireball model, the enhancement is 10%-27% in the same energy range and for zero nadir angle. This enhancement decreases with larger nadir angle, thus providing a novel way to search for $\nu_\tau$ appearance by measuring the angular dependence of the muons. To illustrate how the cascade effect and the $\nu_\tau$ final flux depend on the steepness of the incoming $\nu_\tau$, we show the energy and angular distributions for several generic cases of the incoming tau neutrino flux, $F_\nu^0 \sim E^{-n}$ for n=1,2 and 3.6. We show that for the incoming flux that is not too steep, the signal for the appearance of high-energy $\nu_\tau$ is the enhanced production of lower energy $\mu$ and their distinctive angular dependence, due to the contribution from the $\tau$ decay into $\mu$ just below the detector.

Solar neutrino experiments, GALLEX, SAGE, SNO, SuperK (Jrome Damet)

5.Anything else?