scholarly journals High-energy Neutrino Astronomy: From AMANDA to IceCube

2005 ◽  
Vol 13 ◽  
pp. 13-17
Author(s):  
Francis Halzen
Keyword(s):  
Particle Physics ◽  
Cosmic Ray ◽  
High Energy ◽  
Neutrino Detectors ◽  
First Results ◽  
Cosmic Neutrino ◽  
Observational Fact ◽  
Neutrino Astronomy ◽  
Particle Nature ◽  
Neutrino Fluxes

AbstractKilometer-scale neutrino detectors such as IceCube are discovery instruments covering nuclear and particle physics, cosmology and astronomy. Examples of their multidisciplinary missions include the search for the particle nature of dark matter and for additional small dimensions of space. In the end, their conceptual design is very much anchored to the observational fact that Nature accelerates protons and photons to energies in excess of 1020 and 1013 eV, respectively. The cosmic ray connection sets the scale of cosmic neutrino fluxes. In this context, we discuss the first results of the completed AMANDA detector and the reach of its extension, IceCube.

scholarly journals THE SEARCH FOR NEUTRINO SOURCES BEYOND THE SUN

1996 ◽  
Vol 11 (19) ◽  
pp. 3393-3413 ◽  
Author(s):  
S. BARWICK ◽  
F. HALZEN ◽  
P.B. PRICE
Keyword(s):  
Particle Physics ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Neutrino Telescope ◽  
The Sun ◽  
Electromagnetic Showers ◽  
Electron Neutrinos ◽  
Neutrino Astronomy ◽  
Near Future

It is hoped that in the near future, neutrino astronomy, born with the identification of thermonuclear fusion in the sun and the particle processes controlling the fate of a nearby supernova, will reach throughout and beyond our galaxy and make measurements relevant to cosmology, astrophysics, cosmic-ray physics and particle physics. The construction of a high-energy neutrino telescope requires a huge volume of very transparent, deeply buried material, such as ocean water or ice, which acts as the medium for detecting the particles. The AMANDA1 muon and neutrino telescope, now operating four strings of photomultiplier tubes buried in deep ice at the South Pole, is scheduled to be expanded to a ten-string array. The data collected over the first two years cover the three basic modes in which such instruments are operated: (i) the burst mode which monitors the sky for supernovae, (ii) the detection of electromagnetic showers initiated by PeV-energy cosmic electron neutrinos, and (iii) muon trajectory reconstruction for neutrino and gamma-ray astronomy. We speculate on the possible architectures of kilometer-scale instruments, using early data as a guideline.

scholarly journals Neutrino Telescopes in Antarctica

2000 ◽  
Vol 17 (1) ◽  
pp. 13-17
Author(s):  
Jenni Adams
Keyword(s):  
Particle Physics ◽  
Cosmic Ray ◽  
High Energy ◽  
Neutrino Telescope ◽  
Ocean Water ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Radio Receivers ◽  
Neutrino Astronomy ◽  
Near Future

AbstractIt is hoped that in the near future neutrino astronomy will reach throughout and beyond our galaxy and make measurements relevant to cosmology, astrophysics, cosmic-ray and particle physics. The construction of a high-energy neutrino telescope requires a huge volume of very transparent, deeply buried material such as ocean water or ice, which acts as the medium for detecting the particles. I will describe two experiments using Antarctic ice as this medium: the AMANDA experiment employing photomultiplier tubes and RICE utilising radio receivers.

scholarly journals The Era of Kilometer-Scale Neutrino Detectors

2013 ◽  
Vol 2013 ◽  
pp. 1-20 ◽  
Author(s):  
Francis Halzen ◽  
Uli Katz
Keyword(s):  
Cosmic Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Neutrino Telescopes ◽  
Neutrino Detectors ◽  
Final Design ◽  
Energy Gamma ◽  
Supernova Explosions ◽  
Neutrino Astronomy ◽  
Neutrino Fluxes

Neutrino astronomy beyond the Sun was first imagined in the late 1950s; by the 1970s, it was realized that kilometer-scale neutrino detectors were required. The first such instrument, IceCube, transforms a cubic kilometer of deep and ultra-transparent Antarctic ice into a particle detector. KM3NeT, an instrument that aims to exploit several cubic kilometers of the deep Mediterranean sea as its detector medium, is in its final design stages. The scientific missions of these instruments include searching for sources of cosmic rays and for dark matter, observing Galactic supernova explosions, and studying the neutrinos themselves. Identifying the accelerators that produce Galactic and extragalactic cosmic rays has been a priority mission of several generations of high-energy gamma-ray and neutrino telescopes; success has been elusive so far. Detecting the gamma-ray and neutrino fluxes associated with cosmic rays reaches a new watershed with the completion of IceCube, the first neutrino detector with sensitivity to the anticipated fluxes. In this paper, we will first revisit the rationale for constructing kilometer-scale neutrino detectors. We will subsequently recall the methods for determining the arrival direction, energy and flavor of neutrinos, and will subsequently describe the architecture of the IceCube and KM3NeT detectors.

Detectors for cosmic particles, neutrinos and exotic matter

2020 ◽  
pp. 655-710
Author(s):  
Hermann Kolanoski ◽  
Norbert Wermes
Keyword(s):  
Dark Matter ◽  
Particle Physics ◽  
Cosmic Radiation ◽  
Charged Particles ◽  
Cosmic Ray ◽  
High Energy ◽  
Detection Methods ◽  
Astroparticle Physics ◽  
High Energy Cosmic Rays ◽  
Cosmic Origin

Astroparticle physics deals with the investigation of cosmic radiation using similar detection methods as in particle physics, however, mostly with quite different detector arrangements. In this chapter the detection principles for the different radiation types with cosmic origin are presented, this includes charged particles, gamma radiation, neutrinos and possibly existing Dark Matter. In the case of neutrinos also experiments at accelerators and reactors are included. Examples, which are typical for the different areas, are given for detectors and their properties. For cosmic ray detection apparatuses are deployed above the atmosphere with balloons or satellites or on the ground using the atmosphere as calorimeter in which high-energy cosmic rays develop showers or in underground areas including in water and ice.

scholarly journals Particle Physics with ORCA

2019 ◽  
Vol 207 ◽  
pp. 04003
Author(s):  
Alba Domi ◽  
Simon Bourret ◽  
Liam Quinn
Keyword(s):  
Dark Matter ◽  
Particle Physics ◽  
High Energy ◽  
Neutrino Telescope ◽  
Atmospheric Neutrinos ◽  
Sterile Neutrinos ◽  
Tau Neutrino ◽  
Neutrino Astronomy ◽  
Under Construction

KM3NeT is a Megaton-scale neutrino telescope currently under construction at the bottom of the Mediterranean Sea. When completed, it will consist of two separate detectors: ARCA (Astroparticle Research with Cosmics in the Abyss), optimised for high-energy neutrino astronomy, and ORCA (Oscillation Research with Cosmics in the Abyss) for neutrino oscillation studies of atmospheric neutrinos. The main goal of ORCA is the determination of the neutrino mass ordering (NMO). Nevertheless it is possible to exploit ORCA’s configuration to make other important measurements, such as sterile neutrinos, non standard interactions, tau-neutrino appearance, neutrinos from Supernovae, Dark Matter and Earth Tomography studies. Part of these analyses are summarized here.

scholarly journals The Phenomena of High Energy Astrophysics

2003 ◽  
Vol 214 ◽  
pp. 3-20 ◽  
Author(s):  
R. D. Blandford
Keyword(s):  
Supernova Remnants ◽  
New Technology ◽  
Low Frequency ◽  
Cosmic Ray ◽  
High Energy ◽  
Galactic Cosmic Rays ◽  
High Energy Astrophysics ◽  
Physical Conditions ◽  
Hot Gas ◽  
Neutrino Astronomy

A brief summary of some highlights in the study of high energy astrophysical sources over the past decade is presented. It is argued that the great progress that has been made derives largely from the application of new technology to observation throughout all of the electromagnetic and other spectra and that, on this basis, the next decade should be even more exciting. However, it is imperative to observe cosmic sources throughout these spectra in order to obtain a full understanding of their properties. In addition, it is necessary to learn the universal laws that govern the macroscopic and the microscopic behavior of cosmic plasma over a great range of physical conditions by combining observations of different classes of source. These two injunctions are illustrated by discussions of cosmology, hot gas, supernova remnants and explosions, neutron stars, black holes and ultrarelativistic outflows. New interpreations of the acceleration of Galactic cosmic rays, the cooling of hot gas in rich clusters and the nature of ultrarelativistic outflows are outlined. The new frontiers of VHE γ-ray astronomy, low frequency radio astronomy, neutrino astronomy, UHE cosmic ray physics and gravitational wave astronomy are especially promising.

scholarly journals Distribution of Neutrino Fluxes from Pulsar Shells

1981 ◽  
Vol 94 ◽  
pp. 207-208
Author(s):  
M. M. Shapiro ◽  
R. Silberberg
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Powerful Source ◽  
Stellar Collapse ◽  
Supernova Shell ◽  
Neutrino Fluxes ◽  
Power Outputs ◽  
Initial Power ◽  
Central Pulsar

Young pulsars apparently have a distribution of initial power outputs N (> Po−γ), with 1/2 < γ < 1 and Po ≳ 1038 ergs/sec. Assuming that ultra-high-energy (E ≳ 1015 eV) cosmic-ray nuclei are accelerated at the central pulsar, a young, dense supernova shell can be a powerful source of high-energy neutrinos. With an optical array placed in a volume of one km3 at great ocean depths, as proposed for the DUMAND detector, it is likely that ≳ 103 hadronic and electromagnetic cascades induced by neutrinos would be recorded for a stellar collapse within our Galaxy. Such supernovae occur about 8 times per century. Neutrinos from young supernova shells in the Virgo supercluster would be marginally detectable via neutrinos with N(> Po) ∝ Po−1/2, but unobservable if N(> Po) ∝ Po−1.

scholarly journals PHYSICS WITH COSMIC NEUTRINOS, PEV TO ZEV

2003 ◽  
Vol 18 (22) ◽  
pp. 4065-4083 ◽  
Author(s):  
THOMAS J. WEILER
Keyword(s):  
Cross Section ◽  
Particle Physics ◽  
Statistical Significance ◽  
Cosmic Ray ◽  
New Physics ◽  
Microwave Background ◽  
Radiation Fields ◽  
Cosmic Neutrino ◽  
Long Lifetime ◽  
The Impact

Neutrinos offer a particularly promising eye on the extreme Universe. Neutrinos are not attenuated by intervening radiation fields such as the Cosmic Microwave Background, and so they are messengers from the very distant and very young phase of the universe. Also, neutrinos are not deflected by cosmic magnetic fields, and so they should point to their sources. In addition, there are particle physics aspects of neutrinos which can be tested only with cosmic neutrino beams. After a brief overview of highest-energy cosmic ray data, and the present and proposed experiments which will perform neutrino astronomy, we discuss two particle physics aspects of neutrinos. They are possible long-lifetime decay of the neutrino, and a measurement of the neutrino-nucleon cross-section at a CMS energy orders of magnitude beyond what can be achieved with terrestrial accelerators. Measurement of an anomalously large neutrino cross-section would indicate new physics (e.g. low string-scale, extra dimensions, precocious unification), while a smaller than expected cross-section would reveal an aspect of QCD evolution. We then discuss aspects of neutrino-primary models for the extreme-energy (EE) cosmic ray data. Primary neutrinos in extant data are motivated by the directional clustering at EE reported by the AGASA experiment. We discuss the impact of the strongly-interacting neutrino hypothesis on lower-energy physics via dispersion relations, the statistical significance of AGASA directional clustering, and the possible relevance of the Z-burst mechanism for existing EE cosmic ray data.

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