[en] It is proposed that the decrease in cosmic ray secondary to primary abundances with increasing energy is a natural consequence of the decreasing efficiency of cosmic ray scattering by plasma instabilities. The low streaming velocities that can result might also account for a possible truncation of the pathlength distribution. An idealized model equation is used to illustrate some (eventually) observable consequences of this mechanism

[en] We examine the relative merits and difficulties of the primary and secondary origin hypotheses for the observed cosmic-ray antiprotons, including the new low-energy measurement of Buffington, et al. We conclude that the cosmic-ray antiproton data may be strong evidence for antimatter galaxies and baryon symmetric cosmology. The present antiproton data are consistent with a primary extragalactic component having antip/p approximately equal 3.2+-0.7x10^-4 independent of energy

[en] Even in the absence of antiprotons in the primary cosmic rays, a flux of secondary antiprotons will be produced in collisions between cosmic rays and interstellar gas. The predicted antiproton fraction increases with increasing cosmic-ray confinement, so that observations of antiprotons will provide a probe of models of cosmic-ray confinement. It is shown that the expected antiproton fraction [for E (p-bar) > or approx. =10 GeV] ranges between 2.3 x 10^-4 for the ''leaky box'' model and 18 x 10^-4 for the ''closed box'' model. In addition, attention is called to the fact that a detection of cosmic-ray antiprotons at, or above, a level of 2 x 10^-4 will provide a valuable lower limit to the antiproton lifetime

No abstract available

[en] The relative merits and difficulties of the primary and secondary origin hypotheses for the observed cosmic ray antiprotons, including the low energy measurement of Buffington, were examined. It is concluded that the cosmic ray antiproton data may be strong evidence for antimatter galaxies and baryon symmetric cosmology. The present antiproton data are consistent with a primary extragalactic component having antiproton/proton approximately equal to .0032 + or - 0.7

No abstract available

[en] The data analysis and report of the results of the final charge-ratio experiment using the Utah cosmic-ray muon detector is described. Values for the charge ratio were obtained from least-squares fits to the observed bending-angle distributions. The fitting function was the result of folding the noise scattering distribution into the ideal local-spectrum bending distribution, with the charge ratio as the parameter of the fit. This method permitted a greater precision while circumventing the main causes of charge-ratio dilution. The average value 1.378 +- 0.015 for muon momentum at production between 1 and 8 TeV/c corresponding to a medium primary cosmic-ray momentum range 8 - 61 TeV/c is obtained. With the results of this experiment the charge ratio is precisely known over about three decades of muon energy beginning around 10 GeV. Thus, we believe the charge ratio can serve as a touchstone in determining the hadronic interaction dynamics and composition of the primary cosmic rays. Already approximate agreement has been obtained with experimental results from predictions utilizing the scaling/limiting-fragmentation hypothesis and constant composition of the primary cosmic rays

No abstract available

No abstract available

[en] It is shown that at low energies the depletion of short path lengths in the interstellar cosmic-ray path-length distribution is a function of energy, decreasing in magnitude with increasing energy. The analysis leading to this conclusion is based on the comparison of compiled data for the B/C and sub-Fe/Fe ratios at 0.08--50 GeV per nucleon, with the results of detailed galactic propagation and solar modulation calculations, which include experimental values for the important nuclear cross sections. This energy dependence of the depletion resolves some of the conflicts between previous reports on the question of short path lengths and may be explained by models including a matter distribution around discrete sources or, possibly, by models invoking waves generated by particle-magnetic field interactions in the Galaxy