Trends in Astroparticle-Physics

285 Pages·1994·9.042 MB·German

by  D. Samm (auth.), Prof. Dr. Peter Christian Bosetti (eds.)

TEUBNER-TEXTE zur Physik Band 28
P. C. Bosetti (Hrsg.)
Trends in Astroparticle-Physics
TEUBNER-TEXTE zur Physik
Herausgegeben von
Prof. Dr. Werner Ebeling, Berlin
Prof. Dr. Manfred Pilkuhn, Stuttgart
Prof. Dr. Bernd Wilhelmi, Jena
This regular series includes the presentation of recent research developments
of strong interest as well as comprehensive treatments of important selected
topics of physics. One of the aims is to make new results of research available
to graduate students and younger scientists, and moreover to all people who
like to widen their scope and inform themselves about new developments and
trends.
A larger part of physics and applications of physics and also its application in
neighbouring sciences such as chemistry, biology and technology is covered.
Examples for typical topics are: Statistical physics, physics of condensed mat
ter, interaction of light with matter, mesoscopic physics, physics of surfaces and
interfaces, laser physics, nonlinear processes and selforganization, ultrafast
dynamics, chemical and biological physics, quantum measuring devices with
ultimately high resolution and sensitivity, and finally applications of physics in
interdisciplinary fields.
Trends in
Astroparticle-Physics
Edited by
Prof. Dr. Peter Christian Bosetti
Institute for Physics, Vijlen
Springer Fachmedien Wiesbaden GmbH
Prof. Dr. Peter Christian Bosetti
Born in 1948 in HOekinghausen. Studied physies in Aaehen from 1967 to 1972. Dr. rer.
nat. (1975), Privatdozent (1982), C2 Professor (1987) at RWTH Aaehen, Direktor VIP
(Vijlen) sinee 1991, ApI. Professor for Physies at RWTH Aaehen sinee 1993.
Fields of interest: particle physies, astrophysies, eosmology, biophysies.
Die Deutsche Bibliothek - CIP-Einheitsaufnahme
Trends in astroparticle physics /
ed. by Peter Christian Bosetti.
-Stuttgart ; Leipzig; Teubner, 1994
(Teubner-Texte zur Physik ; 28)
ISBN 978-3-663-01467-6 ISBN 978-3-663-01466-9 (eBook)
DOI 10.1007/978-3-663-01466-9
NE: Bosetti, Peter C. [Hrsg.] ; GT
Das Werk einschlieBlich aller seiner Teile ist urheberrechtlich geschOtzt. Jede Verwertung auBerhalb
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strafbar. Das gilt besonders fOr Vervielfăltigungen, Obersetzungen, Mikroverfilmungen und die Ein
speicherung und Verarbeitung in elektronischen Systemen.
© Springer Fachmedien Wiesbaden 1994
UrsprOnglich erschienen bei B. G. Teubner Verlagsgesellschaft Leipzig 1994
Softcover reprint of the hardcover 1s t edltlon 1994
Umschlaggestaltung: E. Kretschmer, Leipzig
Preface
From October 10 to 12, 1991 the Second International Conference on Trends in
Astroparticle-Physics took place at Aachen, Germany. The meeting was the second in
a series that started in 1990 at UCLA. It was attended by about 100 physicists from
allover the world and covered the interface of elementary particles and astrophysics.
Topics covered included Neutrino-Telescopes in preparation, high energy gamma ray
detectors, cosmology and particle physics, but also new ideas for future detectors.
Many people have worked hard on the preparation for the meeting and deserve many
thanks, in particular D. Rein, L. Sehgal, U. Berson, G. Wurm, C. Wiebusch, C. Ley,
and U. Braun. Representing the conference secretariat, I. Goidie, U. Packbier, and L.
Jenckins were of great help. We also would like to thank the Stadtsparkasse Aachen,
in particular Mr. Fischer, Mrs Cremers and Direktor Schwind for their support and
providing the meeting facilities as well as making possible in parallel a public
exhibition on the topic of the conference. Very special thanks goes to H. Geller,
without whom this conference could not have taken place. Last but not least we wish
to thank the speakers for taking their time in preparing their talks and presenting
their results, making this publication possible.
Amongst the local participants of the conference was also Prof. Helmuth Faissner, not
missing one of the talks. Helmuth Faissner has dedicated his scientific life to
fundamental research keeping always unconventional experiments in mind. With his
great understanding and intuition on elementary particle physics he has influenced a
great number of young (and older) scientists and initiated many important
experiments.
We would like to dedicate these proceedings to Professor Helmuth Faissner to his
65th birthday.
Vijlen, October 1993 Peter Christian Bosetti
Contents
Neutrino-Astrophysics Chair: J. G. Learned
DUMAND and the Search for High Energy Neutrino Point Sources
D. Samm, Aachen .............................. . 9
Physics Capabilities of the Second-Stage Baikal Detector NT-lOO
ell. Spiering, Zellthen . . . . . . . . . . . . . . . . 21
Characteristics of the GALLEX Spectrometer
G. HellSser, Heidelberg ........ . 33
The Sudbury Neutrino Observatory
1. R. Leslie, Kingston 48
Cosmology and Particle Physics Chair: L. Sehgal
Cosmic Particle Dynamics - Acceleration in Spherical Wave Fields
K. O. Thielheim, Kiel 58
Neutrinos from Active Galactic Nuclei
V. 1. Stenger, Hawaii ........... . 70
Characteristics of Cosmological Evolution and Large Scale Structures in The Cosmos
P. Minkowski, Bern 77
The Galaxy Distribution as a Voronoi Foam
V. !eke, Leiden .................. . 89
Contributed Papers Chair: A. Burrows
A Novel Possibility for Neutrino Masses and Decay
S. Barshay, Aachen .................. . . ........................ 107
A Look at Stellar Collapse by Neutral Currents
C. Bemporad, Pisa ............................................... 115
7
NESTOR and SADCO in the Mediterranean
l. M. Zhelezllykh, Moscow ............ . · ........................... 121
The Optical Sensor for the Lake Baikal Project
B. K. Lllbsalldorzhiev, INR, Moscow · ........................... 132
High Energy Gamma Rays Chair: I. M. Zheleznykh
The HEGRA Experiment
E. Lorenz, Mllllich ..... . ................................... 139
Surface Water Cerenkov Detectors
F. BobiSl/t, Padova .......... . · ........................... 152
MACRO at Gran Sasso: Results and Prospects
C. Bemporad, Pisa .................. . . ............. 165
Muons in r·ray Air Showers and the Photoproduction Cross Section
F. Halzell, Wiscollsill . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. 179
Detector Concepts and New Ideas Chair: E. Lorenz
JULIA
P. C. Bosetti, Aachell ..................... 188
AMANDA: Antarctic Muon And Neutrino Detector Array
F. Halzell, WiSCOIlSill .............................................. 211
Contributed Papers Chair: C. Spiering
Signal Processing with JULIA
C. H. V. Wiebllsch, Aachell . . . ............................... 217
Deep-Sea Laboratories for Ocean Sciences
H. BOeker, Kiel . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. 226
8
Summaries Chair: P. C. Bosetti
Neutrino Astrophysics
A. Burrows, Tucson . . . . ............................... 232
Dark Matter and High Energy Neutrinos
V. BerezillSki, Assergi alld Moscow ............................... ' 243
Outlook and Conclusions
D. H. PerkillS, Oxford . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. 265
DUMAND and the search for high energy neutrino point
sources
D. Samm.
III. Physikalisches Institut, Technische Hochschule Aachen, D-5100 Aachen, Germany
presented for the DUMAND Collaboration*
Abstract
DUMAND is a project to build a deep underwater laboratory. The main goal is
to detect and study sources of high energy neutrinos. DUMAND Stage II will consist
of 216 optical modules arranged in nine strings 230 m high in an octagon 105 m in
diameter. The array is to be located approximately 30 km offshore, west of Keahole
Point off the Big Island of Hawaii at an ocean depth of 4.8 km. The array will have
an effective area of 20 000 m2 for throughgoing muons from> 100 GeV neutrinos
of atmospheric and extraterrestrial origin. The angular resolution for reconstructed
muons is 10. The minimum detectable flux from a point source is 1O-lUcm-2s-1 above
1 TeV.
1. Concept of DUMAND
DUMAND (Deep Underwater Muon And Neutrino Detector) is a particle astro
physics experiment, whose major goal is to detect and study sources of high energy
neutrinos. The detection of these high energy neutrinos is based on the fact, that
muons produced via charged current reactions of neutrinos will emit Cherenkov light
while passing through water. This light will be detected by an array of large photo
multipliers with hemispherical photocathodes deployed in the deep ocean.
The signature of a neutrino interaction within or near the DUM AND detector is
a long straight muon from a direction anywhere in the range of 20° above the equator
to straight up through the center of the earth. The direction of the muon track will be
reconstructed from the arrival time of the photomultiplier hits and measured charge.
To search for point sources the experiment must be able to distinguish between
upgoing muons due to the neutrinos searched for and downgoing cosmic ray muons
of much more intense flux. The most physical background comes from upward muons
induced by atmospheric neutrinos. Due to the large area and the good time resolution
of the photomultipliers, which leads to reconstructed muon tracks with high accuracy,
none of these backgrounds should be a problem.
The detector is situated in the deep ocean (4.8 km) to shield it from cosmic
ray backgrounds and utilize seewater as both target and detection medium. Fig. 1
illustrates the concept of DUMA ND. An adequate site to deploy a deep underwater
Cherenkov detector was found in the pacific ocean, 30 km off the Big Island of Hawaii