A cosmic-ray counter telescope for high mass resolution.
Counter telescope consisting of plastic scintillators and NaI crystal to determine charge, mass and energy of low energy cosmic rays
Badhwar, G. D.↗
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Results from the imp 1 gm counter telescope experiment.
Cosmic ray intensity variations measured by GM COUNTER telescope onboard Imp I satellite for study of interplanetary medium
COSMIC RADIATION↗
Cosmic-ray proton and helium spectra and solar modulation effects in the new solar cycle measured with a four-element counter telescope.
Primary cosmic ray proton and He energy spectra and solar modulation effects during sunspot minimum from balloon-borne scintillation counter telescope data
Ormes, J. F.↗
HILT - A heavy ion large area proportional counter telescope for solar and anomalous cosmic rays
The HILT sensor has been designed to measure heavy ion elemental abundances, energy spectra, and direction of incidence in the mass range from He to Fe and in the energy range 4 to 250 MeV/nucleon. With its large geometric factor of 60 sq cm sr the sensor is optimized to provide compositional and spectral measurements for low intensity cosmic rays (i.e. for small solar energetic particle events and for the anomalous component of cosmic rays). The instrument combines a large area ion drift chamber-proportional counter system with two arrays of 16 Li-drift solid state detectors and 16 CsI crystals. The multi dE/dx-E technique provides a low background mass and energy determination. The sensor also measures particle direction. Combining these measurements with the information on the spacecraft position and attitude in the low-altitude polar orbit, it will be possible to infer the ionic charge of the ions from the local cutoff of the Earth's magnetic field. The ionic charge in this energy range is of particular interest because it provides unique clues to the origin of these particles and has not been investigated systematically so far. Together with the other instruments on board SAMPEX (LEICA, MAST, and PET), a comprehensive measurement of the entire solar and anomalous particle population will be achieved.
Klecker, Berndt↗
Multi-channel digital program generator for simulating charged particle penetration of counter telescopes.
Simulation of charged particle penetration in solid state detectors by stimulating them with IR light pulses, examining program generator and switching logic
PARTICLE DETECTOR↗
A scintillation counter telescope for charge and mass indentification of primary cosmic rays
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Bryant, D. A.↗
Composition of cosmic-ray nuclei at high energies.
We have measured the charge composition of cosmic-ray nuclei from Li to Fe with energies up to about 100 GeV/nucleon. A balloon-borne counter telescope with gas Cherenkov counters for energy determination was used for this experiment. Our first results show that, in contrast to low-energy observations, the relative abundances change as a function of energy. We find that the ratio of the galactic secondary nuclei to primary-source nuclei decreases at energies above about 30 GeV/nucleon.
Juliusson, E.↗
The energy spectrum of primary cosmic ray electrons from 2 GeV to 200 GeV.
Use of a balloon-borne counter telescope with a gas Cerenkov counter to measure the energy of primary cosmic ray electrons between 2 and 200 GeV. Electrons are identified by the characteristic electron-photon shower which they produce in a 15 radiation length deep stack of high-Z material interleaved with scintillation counters. Calibrations with monoenergetic electrons up to 14 GeV and monoenergetic protons up to 28 GeV from accelerators are used to develop criteria to statistically separate electrons from proton-induced events. The results from six balloon flights (total exposure time 63 hours) are combined to obtain the electron energy spectrum. Up to about 30 GeV, the spectrum measured in this experiment can be directly checked with calibrations and agrees well with results from other experiments. Above this energy, the flux reported in the present work is somewhat higher than the determinations reported by most other authors. An apparent flattening of the energy spectrum above 50 GeV is not regarded as significant. There is no evidence for a steepening of the spectrum at energies below 200 GeV.
Fanselow, J. L.↗
Cosmic ray nuclear composition above 20 GeV/nucleon
In three balloon flights during 1971 and 1972 a scintillator-Cerenkov counter telescope was exposed for a net total of 7.6 sq m-ster-hr to measure the charge composition of cosmic-ray nuclei. The telescope includes two gas Cerenkov counters for energy measurements above 20 GeV/nucleon. In this energy range about 3400 nuclei between Li and Fe have been detected and analyzed. The resulting charge composition and energy spectra are presented. The nuclear composition has been found to change with energy. The flux of galactic daughter nuclei decreases faster with increasing energy than the flux of source nuclei. The carbon/oxygen abundance ratio is significantly reduced as compared to low-energy measurements, and iron seems to exhibit a flatter energy spectrum than other nuclei.
Juliusson, E.↗
Charge composition and energy spectra of cosmic-ray nuclei at energies above 5 GeV per nucleon
A scintillation-Cerenkov counter telescope, with three gas Cerenkov counters for energy determination between 5 and 90 GeV per nucleon, has been exposed for a net total of 4.5 sq m sr hr in two balloon flights in 1974. The measurement yields the chemical composition and energy spectra of cosmic-ray nuclei in the charge range 5-28. The differential spectral indices of oxygen and of the iron group are measured to be 2.67 plus or minus 0.04 and 2.5 plus or minus 0.08 above 5.4 GeV per nucleon, respectively. The results are interpreted in the context of the 'leaky-box' model of cosmic-ray confinement and propagation.
Caldwell, J. H.↗
Search for 1/3e and 2/3e charged quarks in the cosmic radiation at 2750-m altitude.
A scintillation counter telescope consisting of eight liquid scintillation counters and four wide-gap spark chambers was used to search for particles with electric charge 1/3e and 2/3e in cosmic rays at 2750 m above sea level. No such particles were detected during the 1500-hr experimental run. Upper limits on the vertical fluxes are established, and estimates of the corresponding sea-level fluxes are made for comparison with previous results.
Cox, A. J.↗
High-energy gamma-ray astronomy
The subject of gamma-ray astronomy is discussed with emphasis on celestial gamma rays with energies in excess of 10 MeV. Early observations of such gamma rays are reviewed, a gamma-ray spark-chamber telescope is described together with a gas Cerenkov-counter telescope, and the gamma-ray sky is delineated. It is shown that the diffuse high-energy gamma radiation from the galactic plane probably results primarily from cosmic-ray interactions with interstellar matter. Mechanisms for gamma-ray production are identified, and it is noted that the general galactic radiation may prove to be of great value in studies of galactic structure. Possible sources are considered for the diffuse celestial radiation, and discrete sources are described, including the Crab pulsar, the Vela remnant, the Cygnus region, and Gould's Belt. Future developments in gamma-ray astronomy are considered.
Fichtel, C.↗
Cosmic ray telescope for OGO 2 and 4 spacecraft
The construction and subsequent flight are described of a cosmic ray telescope aboard the OGO-2 and 4 Spacecraft. This instrument was a combination Cerekov-scintillation counter telescope designed to measure the cosmic ray energy spectrum from 1-15 GV and charge composition from Z=1-8. OGO-2 was launched in October 1965; however, attitude control problems caused a rapid loss of control gas, so that after approximately 2 weeks it was no longer possible to point the spacecraft. This mission was officially declared a failure. The cosmic ray instrument appeared to work well during this time. OGO-4 was launched in July 1967, with a similar telescope aboard. It operated successfully approximately one year. The details of the experiment, its operation, and the results are given.
Webber, W. R.↗
The development of a high energy cosmic ray detector for Spacelab-2
A large cosmic ray detector aimed at measurements of the energy spectra and of the elemental abundances of cosmic ray nuclei at very high energies, up to several TeV/nucleon was constructed. The instrument is an electronic counter telescope with a geometric factor of 5 sq ster. It accomplishes measurements of the particle energies through the use of gas Cerenkov counters and of transition radiation detectors. The solutions of a number of technological problems that are encountered when developing such instrumentation for Shuttle missions are discussed.
Lheureux, J.↗
COSMIC RAY EXPERIMENTS FOR EXPLORER XII AND THE ORBITING GEOPHYSICAL OBSERVATORY
Cosmic ray experiments for explorer xii and the orbiting geophysical observatory using geiger- muller counters, and scintillation counter telescopes
COSMIC RADIATION↗
Recent highlights from IceCube
The IceCube Neutrino Observatory, completed in December 2010, is located at the geographic South Pole and incorporates a one cubic kilometer neutrino detector buried in the deep ice and a one square kilometer air shower array, IceTop, sitting atop the glacial ice. This unique combination of neutrino and cosmic-ray detectors allows to investigate a wide variety of physics topics both in astrophysics and particle physics. Here, we discuss latest results from IceCube concentrating on astrophysical aspects.
46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND ↗
GeV neutrinos from collisional heating in GRBs: Detection prospects with IceCube-DeepCore
The observed gamma-ray burst (GRB) emission may be due to jet reheating via nuclear collisions. The role of this collisional heating can be probed through the observation of 10–100 GeV neutrinos, which are generated in nuclear collisions along with gamma rays. Neutrino and gamma-ray luminosities are closely related, which further aids observations. If the main mechanism behind the production of GRBs is collisional heating then IceCube-DeepCore could detect the GeV-neutrino emission of GRBs with a few years of observation.
46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND ↗
Low-energy neutrino search for dark matter in the Galactic Center with IceCube-DeepCore
The cubic-kilometer sized IceCube neutrino observatory, constructed in the glacial ice at the South Pole, offers new opportunities for neutrino physics to reach lower neutrino energies with its in-fill array 'DeepCore'. A set of analysis techniques where the outer layers of IceCube are used as a veto makes it possible to reject atmospheric muons and thereby allows low-energy neutrino searches to be performed above the horizon. With these techniques the Galactic Center, an important target in searches for self-annihilating dark matter, becomes accessible for IceCube. In this contribution, we present the status of the Galactic Center dark matter analysis, using more than 10 months of data taken with the 79-string configuration of IceCube-DeepCore, as well as the new veto techniques used in the analysis.
46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND ↗