Calculations of the propagation of UH-nuclei were improved by extending the number of individual nuclides considered, and by using more recent evaluations of the rigidity dependence of the escape length, the possible source composition, and altered cross sections. The effects of using different expressions for the dependence of abundances on first ionization potentials (FIP) are outlined. The sensitivity of the calculated elemental abundances to the various changes made in the propagation assumptions are discussed
Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 ≤ Z ≤ 40 ha...
The fragmentation of 10.6 GeV/n Au in CH_2. C, Al, Cu, Sn, and Pb targets has been studied using an ...
The cosmic ray abundances have traditionally been used to determine the elemental and isotopic natur...
The HEAO-3 Heavy Nuclei Experiment has measured elemental abundances of ultraheavy cosmic rays near...
The suggestions that the source abundances of cosmic ray nuclei heavier then Fe differ significantly...
Analysis of a new, higher resolution data set from the Heavy Nuclei Experiment on the HEA0-3 spacec...
The observed fluxes of cosmic ray (C.R.) ultraheavy elements depend on their charge and mass spectru...
We report here an analysis that, for the first time, systematically normalizes the data from the HEA...
The relative abundance of nuclear species measured in cosmic rays at Earth has often been interprete...
Over the past few years, we have been analyzing the HEAO-3 measurements of the abundances of ultra-...
We have examined relativistic nuclei of iron, krypton, xenon, holmium and gold, accelerated to maxi...
Over the past few years, the HEAO-3 measurements of the abundances of ultra-heavy cosmic ray nuclei ...
We present the results on the source spectrum function for primary nuclei in galactic cosmic rays, w...
An assessment is given of the galactic cosmic ray source (GCRS) elemental composition and its correl...
Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 ≤ Z ≤ 40 ha...
Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 ≤ Z ≤ 40 ha...
The fragmentation of 10.6 GeV/n Au in CH_2. C, Al, Cu, Sn, and Pb targets has been studied using an ...
The cosmic ray abundances have traditionally been used to determine the elemental and isotopic natur...
The HEAO-3 Heavy Nuclei Experiment has measured elemental abundances of ultraheavy cosmic rays near...
The suggestions that the source abundances of cosmic ray nuclei heavier then Fe differ significantly...
Analysis of a new, higher resolution data set from the Heavy Nuclei Experiment on the HEA0-3 spacec...
The observed fluxes of cosmic ray (C.R.) ultraheavy elements depend on their charge and mass spectru...
We report here an analysis that, for the first time, systematically normalizes the data from the HEA...
The relative abundance of nuclear species measured in cosmic rays at Earth has often been interprete...
Over the past few years, we have been analyzing the HEAO-3 measurements of the abundances of ultra-...
We have examined relativistic nuclei of iron, krypton, xenon, holmium and gold, accelerated to maxi...
Over the past few years, the HEAO-3 measurements of the abundances of ultra-heavy cosmic ray nuclei ...
We present the results on the source spectrum function for primary nuclei in galactic cosmic rays, w...
An assessment is given of the galactic cosmic ray source (GCRS) elemental composition and its correl...
Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 ≤ Z ≤ 40 ha...
Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 ≤ Z ≤ 40 ha...
The fragmentation of 10.6 GeV/n Au in CH_2. C, Al, Cu, Sn, and Pb targets has been studied using an ...
The cosmic ray abundances have traditionally been used to determine the elemental and isotopic natur...