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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Low energy cosmic ray modulation relationship to observed interplanetary magnetic field irregularities in terms of diffusion, using space probes
Spectroscopic evidence on helium abundance of stars in galactic halo
Celestial X-ray sources at low galactic longitude located by rocket observation
Source spectra and composition of galactic cosmic rays implied by analysis of interstellar and interplanetary travel, noting solar modulation
Balloon and satellite measurements of low energy galactic cosmic rays
Haystack Millstone interferometer system for high resolution radiometric studies
Galactic deuterium and energy spectrum above 20 mev per nucleon measured by IMP-III satellite near minimum solar activity
Correlation between position and red shift of quasars indicating anisotropic universe or galactic origin of quasars
Quark radio wave line detection from quasars in galaxies with history of high intensity cosmic rays
Spiral and irregular galaxies total mass to neutral hydrogen mass ratio derived from mass- luminosity relations
Interstellar gas dynamics suggests that energy density of galactic cosmic rays places firm upper limit on undetermined constant of solar modulation
Solar and galactic particle spectra and composition measured with cosmic ray telescope mounted on satellite
Energy spectra measurements of hydrogen and helium isotopes of galactic cosmic radiation, and isotopic composition data interpretation
Extraterrestrial sources radiation including galactic, solar and magnetospheric radio emissions observed by RAE-I satellite at long wavelengths
Observations of galactic center radiation and possible point sources obtained by gamma ray telescope flown on three balloon flights
The spectrum of cosmic ray electrons above 10 GeV was studied extensively. The spectrum is predicted to steepen at an energy which is related to the lifetime of electrons in the interstellar medium against losses due to inverse Compton collisions with photons and to synchrotron radiation in galactic magnetic fields. The experimental results diverge widely; the lack of agreement between the various measurements is due to a variety of experimental problems.
Measurement of the abundances of the nuclei C, N, O, Ne, Mg, Si, Ar, and Ca and the group Cr-Co relative to oxygen from seven solar energetic-particle events in the energy range from about 14 to 61 MeV per nucleon with a solid-state detector telescope on the OGO-5 satellite, 1968-1971. The differential energy spectra of O (14 to 29 MeV per nucleon) and Cr-Co (3 to 61 MeV per nucleon) have a spectral index of about (-3) for a power law in kinetic energy. The relative abundances of C, N, O, and Ne are in excellent agreement with emulsion studies. However, when compared with the solar photospheric and coronal abundances, the OGO-5 measurements show a large enhancement of relative abundances beginning with Si, and extending to the Cr-Co group. The enhancement over the solar and universal abundances is in rough agreement with the composition of the galactic cosmic radiation.
Measurements using a balloon-borne ionization spectrometer on the differential energy spectra of the heavy nuclei of the galactic cosmic radiation are reported. The spectra of individual elements up to oxygen and groups of nuclei up through iron were measured up to almost 100 GeV/nucleon. The energy spectrum of the secondary nuclei, B+N, is steeper than that of the primary nuclei, C+O, by gamma = 0.21 + or - .09 in agreement with other authors. The spectral shapes found are reasonably well represented by single power laws between 2 and 60 GeV/nucleon. Data are consistent with the decrease in the secondary to primary ratio found by others above 20 GeV/nucleon, but it shows no evidence for any sudden change in this ratio within counting statistics. The most dramatic finding is that the spectrum of the iron nuclei is flatter than that of the carbon and oxygen nuclei by 0.57 + or - 0.14 of a power. The experimental techniques for charge and energy determination are presented and corrections due to nuclear disintegration and losses of energy out the bottom of the spectrometer are discussed.