On the detection of ultra high energy neutrinos with the Auger observatory

Capelle, K.; Cronin, J. W.; Parente, G.; Zas, E.

doi:10.1016/s0927-6505(97)00059-5

Cited by 198 publications

(240 citation statements)

References 22 publications

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“…Neutrino fluxes from radio-quiet and radio-loud active galactic nuclei have also been estimated by Mannheim (1995). All channels of neutrino production discussed hitherto have been summarized by Capelle et al(1998).…”

Section: E Neutrinos and Gamma Raysmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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The authors define ''ultrahigh-energy cosmic rays'' (UHECRs) as those cosmic rays with energies above 10 18 eV. It had been anticipated that there would be a cutoff in the energy spectrum of primary cosmic rays around 6ϫ10 19 eV induced by the interaction of the particles with the 2.7-K primordial photons. However, recent experimental data have established that particles exist with energies greatly exceeding this. It follows that the sources of such particles are probably nearby, on a cosmological scale. However, although the trajectories of such energetic particles through the galactic and intergalactic magnetic fields may be nearly rectilinear, no astronomical sources have as yet been identified. This is the enigma of the highest-energy cosmic rays. The paper reviews the history of research in this energy regime and critically assesses the observational results on the energy spectrum, arrival directions, and composition of the primary cosmic rays based on observations made by six experiments. The detection methods currently available are described. Special techniques have been developed as particles of 10 20 eV or higher occur at a rate of only about 1 per km 2 per century. Errors in measurement are given particular attention. The authors also review the theoretical predictions for a number of candidate sources of cosmic rays beyond the predicted cutoff. Finally, the four major projects planned to address the question of the origin of UHECRs are briefly described. CONTENTS

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Section: E Neutrinos and Gamma Raysmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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“…Effective apertures for Auger have been calculated in Ref. [15]. For AGASA, we adopt the Auger aperture for quasi-horizontal EM showers with axes falling in the array, reduced by a factor of 30, the ratio of surface areas of the arrays.…”

Section: Neutrino Exposurementioning

confidence: 99%

Neutrino bounds on astrophysical sources and new physics

et al. 2002

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Ultra-high energy cosmic neutrinos are incisive probes of both astrophysical sources and new TeV-scale physics. Such neutrinos would create extensive air showers deep in the atmosphere. The absence of such showers implies upper limits on incoming neutrino fluxes and cross sections. Combining the exposures of AGASA, the largest existing ground array, with the exposure of the Fly's Eye fluorescence detector integrated over all its operating epochs, we derive 95% CL bounds that substantially improve existing limits. We begin with model-independent bounds on astrophysical fluxes, assuming standard model cross sections, and model-independent bounds on new physics cross sections, assuming a conservative cosmogenic flux. We then derive model-dependent constraints on new components of neutrino flux for several assumed power spectra, and we update bounds on the fundamental Planck scale M D in extra dimension scenarios from black hole production. For large numbers of extra dimensions, we find M D > 2.0 (1.1) TeV for M min BH = M D (5M D ), comparable to or exceeding the most stringent constraints to date.

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“…These include the detection of particle shower fronts in the atmosphere in the horizontal direction (Horizontal Air Showers) [3] and coherent pulses from showers in different media, both acoustic [4] and in radio [4,5] waves. Shower detection is sensitive both to neutral current interactions and to all neutrino flavors.…”

Section: Introductionmentioning

confidence: 99%