HE Neutrinos workshop

Overview

V. Berezinsky, Laboratori Nazionali del Gran Sasso

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Neutrino Interactions with Matter

M.H. Reno, University of Iowa

Neutrino interactions in the Earth affect neutrino fluxes arriving at underground detectors. The differences between muon neutrino and tau neutrino attenuation will be emphasized. Tau lepton electromagnetic energy loss will also be discussed.

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A. Gazizov, Institute of Physics Of the National Academy of Sciences of Belarus

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V. Ptuskin, IZMIRAN

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Neutrino-Nucleon Cross-Section in Extra Dimensions

M. Kachelriess, MPI

After a short introduction of the large extra-dimension scenario, I review experimental constraints thereon. Then I discuss how t-channel exchange of Kaluza-Klein gravitons enhances the neutrino-nucleon cross-section and the implications for experiments like AUGER. Finally, I review the speculations that black hole production can be observed in neutrino telescopes.

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High Energy Neutrinos from GRBs

D. Guetta, Osservatorio Astrofisico Arcetri

Observations imply that gamma-ray bursts (GRBs) are produced by the dissipation of the kinetic energy of a highly relativistic fireball. Photo-meson interactions of protons with gamma-rays within the fireball dissipation region are expected to convert a significant fraction of the fireball energy into high energy neutrinos. In this talk we summarize the results of an analysis of the internal shock model of GRBs, where production of synchrotron photons and photo-meson neutrinos with energies  about 10¹⁴ eV are self-consistently calculated. These neutrinos will be coincident with the GRB. We show that the fraction of fireball energy converted into high energy neutrinos is not sensitive to uncertainties in the fireball model parameters, such as the expansion Lorentz factor and characteristic variability time. Other processes of neutrinos emission from GRBs are also reviewed. Photomeson interactions within the plasma region shocked by the reverse shock, may produce a burst of 10¹⁸ eV neutrinos following the GRB on the time scale of 10 s. Planned 1 km³ neutrino telescopes are expected to detect ten 100 TeV neutrino events and several 10¹⁸ eV events, correlated with GRBs, per year. 

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Hidden High-Energy Neutrino Sources

V. Dokuchaev, Institute for Nuclear Research, Moscow

Review of astrophysical models for `hidden' high-energy (HE) neutrino sources, which are nontransparent for primary cosmic rays (CRs) and accompanied gamma-radiation. HE neutrinos are produced in astrophysical sources as secondaries after primary CR interactions with ambient radiation or matter. As a result the HE neutrino flux is strongly limited by observations of primary CR and/or gamma-ray fluxes from transparent sources. Otherwise the fluxes of HE neutrinos from hidden sources are free this limitation. The predicted fluxes for some types of hidden sources may be high enough for direct observations of separate sources by large neutrino telescopes. This provides the unique opportunity for using neutrino channel for the investigation of `inner engine' operation in hidden sources.

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Gamma Ray Bursts from the First Stars: Neutrino Signal

D. Guetta, Osservatorio Astrofisico Arcetri

If the first (PopIII) stars were very massive, their final fate is to collapse into very massive black holes. Once a proto-black hole has formed into the stellar core, accretion continues through a disk. It is widely accepted, although not confirmed, that magnetic fields drive an energetic jet which produces a burst of TeV neutrinos by photon-meson interaction, and eventually breaks out of the stellar envelope appearing as a Gamma Ray Burst (GRB). In this talk I will show  the results for  the expected neutrino diffuse flux from these PopIII GRBs obtained considering cosmological/stellar simulations and neutrino emission models. The  comparison of these results with the capabilities of present and planned detectors as AMANDA and IceCube allow to derive important informations on the characteristic explosion energies of PopIII GRBs and  on the redshift z_f that marks the metallicity-driven transition from a top-heavy to a normal IMF.

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Atmospheric Neutrinos

P.Lipari, INFN Roma

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Super-heavy Dark Matter and High Energy Neutrinos

I. Tkachev, CERN

Super-heavy Dark Matter (SHDM) is motivated both cosmologically and astrophysically. Namely, if super-heavy particles exist, they are inevitably created in appropriate amounts by simple physical processes in the early Universe.  If super-heavy particles are unstable but long-living, they can provide nice solution to Greisen-Zatsepin-Kuzmin puzzle of UHECR. After reviewing both issues I shall discuss observational signatures, and in particular, neutrino spectra and fluxes predicted in the models of decaying SHDM.

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Z. Berezhiani, Univ. L'Aquila and LNGS

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Ultra High Energy Neutrino Z-Showering , GZK Neutrinos and Horizontal Tau Airshowers

D. Fargion, University of Roma and INFN

The possibility to overcome the GZK cut-off by the Z Showering of ZeV neutrinos onto relic light ones (eV)  offer at once the possibility to understand the UHECR  spectra and their angular correlation with far cosmic BL Lacertae sources. The same Z-Showering may produce rare gamma tails at TeVs overcoming also the Infrared - TeV cut-off for  sources at  large distances. To probe  this model we suggest to observe the Horizontal Tau Airshowers arising copiously at the edge of the Earth by Ultra High GZK neutrino tangent to terrestrial crust.

Mr. Fargion did not want to give his transparancies, instead he gave the code of two papers in which most of his talk is covered: 

• astro-ph/0002453
• hep-ph/0112014

These papers do not contain the pictures and plots, these have to be obtained from the JPEG-format-link provided in the papers.

Neutrino Signals from Observed Microquasars

D. Guetta, Osservatorio Astrofisico Arcetri

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S. Basa, last update: 03/12/02