Relative abundances of elements (20 or = Z or = 28) at energies up to 70 GeV/amu using relativistic rise in ion chambers

The results of a new balloon borne cosmic ray detector flown from Palestine, TX in Sept., 1982 are discussed. The exposure of 62 square meter-ster-hr is sufficient to prove the concept of using gas ionization chambers as energy measuring devices in the relativistic rise region. The abundances, relative Fe-26, of the pure secondaries Cr-22 and Ti-24, the pure primary Ni26, and the mixed primary and secondary Ca-20 between 6 and 70GeV/amu were measured

Energy spectra of elements with 18 or = Z or = 28 between 10 and 300 GeV/amu

The HEAO-3 Heavy Nuclei Experiment is composed of ionization chambers above and below a plastic Cerenkov counter. The energy dependence of the abundances of elements with atomic number, Z, between 18 and 28 at very high energies where they are rare and thus need the large area x time are measured. The measurements of the Danish-French HEAO-3 experiment (Englemann,, et al., 1983) are extended to higher energies, using the relativistic rise of ionization signal as a measure of energy. Source abundances for Ar and Ca were determined

A Bevalac Calibration of a Scintillating Optical Fiber Hodoscope for Possible use on the Advanced Composition Explorer

As part of instrument definition activities for the Advanced Composition Explorer (ACE) we are evaluating a hodoscope comprised of scintillating fibers for possible use in the Cosmic Ray Isotope Spectrometer (CRIS). The hodoscope would determine the trajectories of individual cosmic ray nuclei which stop in the silicon solid state telescopes in CRIS. We report a preliminary analysis of data from a Dec., 1990 Bevalac calibration of a CRIS test model which consisted of a scintillating fiber hodosccpe, utilizing 200mm, square cross section scintillating fibers, and silicon detectors for dE/dx-Erot measurements. The positional resolution obtained in our preliminary data analysis is -60μm for angles from 0-30°. The detection efficiency for iron and silicon nuclei was determined to be >99% for beam angles of ≥ 20°

Energy Spectra of Elements with 18 ≤ Z ≤ 28 Between 10 and 300 GeV/amu

The HEAO-3 Heavy Nuclei Experiment (Binns, et al., 1981) is composed of ionization chambers above and below a plastic Cherenkov counter. We have measured the energy dependence of the abundances of elements with atomic number, Z, between 18 and 28 at very high energies where they are rare and thus need the large area x time of this experiment. We extend the measurements of the Danish French HEAO-3 experiment (Englemann, et al., 19S3) to higher energies, using the relativistic rise of ionization signal as a measure of energy, and determine source abundances for Ar and Ca

Cosmic-Ray Energy Spectra Between Ten and Several Hundred GeV/amu for Elements from _(18)Ar to _(25)Ni--Results from HEAO-3

Using the relativistic rise of energy loss as a measure of energy, we have determined the energy dependence of the abundances relative to _(26)Fe of the elements _(18)Ar, _(19)K, _(20)Ca, _(21)Sc, _(22)Ti, _(23)V, and _(28)Ni, from 10 to several hundred Ge V /amu. From the energy dependence of the observed Ar/Fe and Ca/Fe ratios we infer primary source ratios for these elements

Cosmic-ray energy spectra between 10 and several hundred GeV per atomic mass unit for elements from _(18)Ar to _(28)Ni - Results from HEAO 3

The Heavy Nuclei Experiment on HEAO 3 included ionization chambers and a Cherenkov detector. For nuclei that arrive at locations and from directions with high geomagnetic cutoff ( > 8 GV) the Cherenkov signal determines the atomic number, Z, while the relativistic rise in ionization provides a measure of the energy. For the secondary cosmic-ray elements, _(19)K, _(21)Sc, _(22)Ti, and _(23)V, the abundances relative to _(26)Fe fall as power laws in energy; combining our results from 10 to ~200 GeV per amu with data between 1 and 25 GeV per amu from another instrument on the same spacecraft gives exponents -0.31 ± 0.01, -0.25 ± 0.02, -0.28 ± 0.01, and -0.23 ± 0.02, respectively. For _(28)Ni, which like _(26)Fe is a primary element, the abundance relative to _(26)Fe is essentially independent of energy over the interval from ~10-500 GeV per amu. The elements _(18)Ar and _(20)Ca, which at a few GeV per amu are mixtures of primary and secondary components, display abundances relative to _(26)Fe which fall with increasing energy up to ~100 GeV per amu and then level off at higher energies; from the energy dependence of these abundance ratios we infer Ar/Fe and Ca/Fe ratios in the source of 2.6 ± 0.7% and 8.8 ± 0.7%, respectively

Energy Spectra of Ultraheavy Cosmic Rays Results from HEAO-3

The HEAO-3 Heavy Nuclei Experiment measures cosmic-ray energy directly in the interval 400 to ~1200 MeV/amu. Geomagnetic cutoffs can also be derived up to ~15 GV. We present preliminary rigidity spectra of various ultraheavy cosmic-ray elements relative to iron

The Cosmic-Ray Abundances of the Platinum-Lead Elements as Measured on HEAO-3

The relative abundances of elements in the charge ranges of 75 ≤ Z ≤ 79 (platinum) and 80 ≤ Z ≤ 83 (lead) should be a sensitive indication of the contributions of the r- and s-processes in nucleosynthesis. Data from the HEAO 3 Heavy Nuclei Experiment are used to establish abundances, relative to iron, of these elements in the cosmic radiation, as well as the ratio of 'secondary' elements, in the 62 ≤ Z ≤ 74 range, to the primary lead-platinum elements. These results appear to suggest that either the source abundances are deficient in s-process elements or that they are not organized solely by first ionization potential. In addition, present propagation models can adequately represent the relative abundances of primary and secondary elements