Cosmic ray experiments /elementary particle physics/ in a manned orbiting laboratory
High energy cosmic ray experiments in manned orbiting laboratory
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Phase partitioning, crystal growth, electrodeposition and cosmic ray experiments in microgravity
Five experiments are contained in one Get Away Special Canister (5 cu ft). The first utilizes microgravity to separate biological cells and to study the mechanism of phase partitioning in 12 separate cuvettes. Two experiments are designed to grow organic crystals by physical vapor transport. One experiment consists of eight electroplating cells with various chemicals to produce surfaces electroplated in microgravity. Some of the surfaces have micron sized particles of hard materials co-deposited during electrodeposition. The fifth experiment intercepts cosmic ray particles and records their paths on photographic emulsions. The first four experiments are controlled by an on-board C-MOS controller. The fifth experiment is totally passive. These are the first in Space. Their purpose is to create new commercial products with microgravity processing.
Wessling, Francis C.↗
MDAC solar cosmic ray experiment on OGO-6
The instrumentation of the OGO-F solar cosmic ray experiment is described and results of data obtained during the satellite lifetime from launch on June 5, 1969, through September, 1970, and discussed.
Masley, A. J.↗
Definition study for an advanced cosmic ray experiment utilizing the long duration exposure facility
To achieve the goals of cosmic ray astrophysics, an ultraheavy cosmic ray experiment on an LDEF reflight should be in an orbit with high inclination (approximately 57 deg) at approximately 230 nm for approximately 2 years near solar minimum (approximately 1986). It should fill 61 trays. Each tray should contain 4 modules of total active area 0.7 sq m, with a thermal blanket, thermal labyrinth mounts, aluminum honeycomb mechanical support, and total weight approximately 100 kg. Each module should contain interleaved CR39, Lexan, and thin copper sheets plus one event-thermometer canned in a thin metal cannister sealed with approximately 0.2 atm dry O2. The CR39 and Lexan should be manufactured to specifications and the sheet copper rolled to specifications. The event-thermometer should be a stiffened CR39 sheet that slides via bimetal strips relative to fixed CR39 sheet so that stack temperature can be read out for each event. The metal cannister can be collapsed at launch and landing, capturing the sliding assembly to prevent damage. An engineering study should be made of a prototype LDEF tray; this will include thermal and mechanical tests of detectors and the event thermometer.
Price, P. B.↗
The medium energy cosmic ray experiment for ISEE-C
A description is provided of the medium energy cosmic ray experiment on board the ISEE-C spacecraft. This experiment is designed to measure the charge composition of nuclear energetic particles over wide ranges in energy (1-500 MeV/nucleon) and in charge (Z equals 1-28). Individual isotopes are resolvable for Z equals 1-7 over a restricted energy range. Electrons of 2-10 MeV are measured as well. These measurements are accomplished using all solid-state detector telescopes with detectors ranging in thickness from 15-3000 microns. The scientific goals of the experiment are also described. These include study of the composition of energetic particles from the sun and from the galaxy, the acceleration and flow of particles in the interplanetary medium, and electrons from Jupiter. Heliospheric gradients and other characteristics of solar modulation will be measured in conjunction with identical telescopes flown on the Voyager 1 and 2 spacecraft and similar telescopes on Pioneer 10 and 11.
Von Rosenvinge, T. T.↗
Sonic spark chambers for cosmic-ray experiments
The sonic spark chamber provides an attractive high resolution hodoscope for low flux cosmic ray experiments. Spark position is determined by measurement of the time of flight of the sonic shock front from the spark position to a number of piezoelectric transducers placed at the periphery of the chamber. For each spark, four quantities must be determined: the spark coordinates, the sound velocity, and the spark 'size'. By over-determining the four parameters, high accuracy is possible. With eight sonic transducers, air-gap spark positions were measured with an error of less than 100 microns everywhere over a 1 sq m region.
Ahlen, S. P.↗
Cerenkov light collection in the high energy astronomical observatory - A cosmic ray experiment.
Review of some of the problems encountered in the development of an improved Cerenkov counter for high energy cosmic ray experiments, and discussion of the approaches used or contemplated for the solution of these problems. The solution is felt to be contingent upon a better UV-reflecting paint and an improved radiator and photomultiplier positioning.
Arens, J. F.↗
Exhibit A - statement of work, principal investigator services for the lunar surface cosmic ray experiment, attachment 3
Principal investigator requirements for lunar module-borne cosmic ray detector experiment
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A 100,000 pulse height analyzer for use in High Energy Cosmic Ray Experiments (HECRE) on high altitude balloon flights
A description is given of a wide dynamic range pulse height analyzer system developed for use on High Energy Cosmic Ray Experiment (HECRE) Balloon Flights. A wide dynamic range of 100,000 is obtained by extending the range of a basic 1024 channel analyzer through the use of multiple ranges and range selection. The system described here contains four 100,000 pulse height analyzers. Each 100,000 pulse height analyzer consists of a group of cordwood welded modules mounted and interconnected on a printed circuit card. Four of these card assemblies, the required clock drive circuitry (discrete components mounted and interconnected on a separate card) and three input-output connectors are interconnected and mounted on the system board.
Cancro, C. A.↗
Effect of the Mott cross section on charge identification in the HEAO-3 Heavy Cosmic Ray Experiment
Corrections to the Z-squared dependence of ion chamber and Cherenkov response due to the Mott cross section are calculated for the HEAO-3 Heavy Cosmic Ray Experiment. The effect of the production and escape of high energy secondary electrons on detector response is accounted for by numerical calculations. These secondary electron effects are shown to influence the size of the non Z-squared effects and thus affect the charge assignments and detector resolution. The Bloch and relativistic Bloch corrections are not included in the results presented here but may be combined with the Mott corrections when the Bloch corrections are properly evaluated.
Derrickson, J. H.↗
Cosmic ray experiments source-encoding in the IMP-I spacecraft.
Cosmic ray detectors design for medium, low and very low energy events on IMP-1 spacecraft, noting PCM format
Cancro, C. A.↗
A low-energy solar cosmic ray experiment for OGO-F
Instrumentation data for low energy solar cosmic ray measurements using OGO-F satellite
Burtis, D. W.↗
Results from the Helios galactic and solar cosmic ray experiment (E7)
Energy spectra, charge composition, and flow patterns of solar and galactic cosmic rays were investigated using three nuclear-particle telescopes on Helios to measure electrons (50 keV to 8 MeV) protons (100 eV to 800 MeV) alpha particles (to 600 MeV per nucleon) heavier elements up to neon, (to 200 MeV per nucleon). The experiment includes a proportional counter to monitor solar X-rays in the range 2 to 8 keV. A collection of solar flare associated particle events are observed whereby coronal effects and spatial distribution of flare particles are determined over almost a whole solar cycle; a typical solar particle events are also observed. Earlier explanations concerning corotating energetic particle streams in the inner and outer solar system are confirmed. Solar modulation of galactic cosmic rays is identified. Gamma ray bursts are detected and the sources in the sky are precisely determined, proving the suspected galactic origin.
Trainor, J. H.↗
Cosmic Ray Experiments and the Implications for Indirect Detection of Dark Matter
Detection of cosmic-ray antiprotons was first reported by Golden et al. in 1979 and their existence was firmly established by the BESS and IMAX collaborations in the early 1990s. Increasingly precise measurements of the antiproton spectrum, most recently from BESS-Polar and PAMELA, have made it an important tool for investigating cosmic-ray transport in the galaxy and heliosphere and for constraining dark-matter models. The history of antiproton measurements will be briefly reviewed. The current status will be discussed, focusing on the results of BESS-Polar II and their implications for the possibility of antiprotons from primordial black hole evaporation. The current results of the BESS-Polar II antihelium search are also presented.
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Large area ion chambers for a high energy cosmic ray experiment
High resolution measurement of the iron group nuclei was performed with the intention of determining individual abundances in the cosmic ray flux at the earth of particles with z = 22 to 30. Of the three types of dE/dx detectors used in the experiment, pulse ion chambers, Cerenkov radiators and scintillators, the first has the best z resolution over a wide range of particle z and energy. The plastic scintillators define the particle acceptance cone of the telescope while the Cerenkov detector aids in rejection of low energy particle background and measurement of particle velocity.
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Lunar surface cosmic ray experiment S-152, Apollo 16
This investigation was directed at determining the energy spectra and abundances of low energy heavy cosmic rays (0.03 E or = 150 MeV/nucleon). The cosmic rays were detected using plastic and glass particle track detectors. Particles emitted during the 17 April 1972 solar flare dominated the spectra for energies below about 70 MeV/nucleon. Two conclusions emerge from the low energy data: (1) The differential energy spectra for solar particles vary rapidly for energies as low as 0.05 MeV/nucleon for iron-group nuclei. (2) The abundance ratio of heavy elements changes with energy at low energies; heavy elements are enhanced relative to higher elements increasingly as the energy decreases. Galactic particle fluxes recorded within the spacecraft are in agreement with those predicted taking into account solar modulation and spacecraft shielding. The composition of the nuclei at energies above 70 MeV/nucleon imply that these particles originate outside the solar system and hence are galactic cosmic rays.
Fleischer, R. L.↗
Data processing for a cosmic ray experiment onboard the solar probes Helios 1 and 2: Experiment 6
The data processing system for the Helios experiment 6, measuring energetic charged particles of solar, planetary and galactic origin in the inner solar system, is described. The aim of this experiment is to extend knowledge on origin and propagation of cosmic rays. The different programs for data reduction, analysis, presentation, and scientific evaluation are described as well as hardware and software of the data processing equipment. A chronological presentation of the data processing operation is given. Procedures and methods for data analysis which were developed can be used with minor modifications for analysis of other space research experiments.
Mueller-Mellin, R.↗
Project BIOCORE /M212/, a biological cosmic ray experiment - Procedures, summary, and conclusions
The primary objective of the experiment was to determine whether a specific portion of the high Z-high energy (HZE) galactic cosmic ray particle spectrum, especially particles with Z no less than 6, can produce microscopically visible injury of brain and eye tissues. Pocket mice (Perognathus longimembris), obtained from the California desert, were selected as the biological target. Five of these mice were flown on Apollo XVII. Not only the brain and eyes but also many other tissues of these animals were studied for evidence of cosmic ray particle damage. The lack of prior experimental evidence as to the character of the potential injury induced by HZE particles required reliance on the physical characteristics of particle radiation in ascertaining the probable nature of the injury. These characteristics and the key aspects of the experiment are summarized in this paper. Subsequent articles in this special supplement give details of the biological, engineering, and dosimetric aspects of BIOCORE together with the results.
Haymaker, W.↗