Studies of the chemical composition of cosmic rays withZ=3 30 at high and low energies

Details Studies of the chemical composition of cosmic rays withZ=3 30 at high and low energies Studies of the chemical composition of cosmic rays withZ=3 30 at high and low energies

Feb 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..15..245w&link_type=abstract

Astrophysics and Space Science, Volume 15, Issue 2, pp.245-271

Astronomy and Astrophysics

Astrophysics

56

Scientific paper

We have measured the chemical composition of cosmic rays withZ≥2 over an energy range from ˜100 MeV/nuc to >2 GeV/nuc using 2 new large area counter telescopes. One of these instruments was a 4 element dE/dx×E× Range telescope, the other a 4 element dE/dx×Cerenkov× ×Range telescope. Two balloon flights with these telescopes at Ft. Churchill in the summer of 1970 provided a total of nearly 1000 Fe nuclei with a charge resolution ranging from ˜0.10 charge unit at Carbon to ˜0.25 charge unit at Fe. A detailed charge spectrum is obtained at both high and low energies. Some important differences exist between the present results and those obtained earlier, due in part to the improved statistical accuracy and in part to the improved background rejection of the present data. In particular, the abundance of Cr and Mn are each found to be ˜0.10×Fe in contrast to the earlier ratio of ˜0.30 found by some workers for each of these nuclei. The abundance of these two nuclei, as well as others in the 15 25 range, shows no strong dependence on energy. We have extrapolated our composition data to the cosmic ray sources using a variety of interstellar path length distributions. The abundances ofall secondary nuclei withZ between 3 25 are consistent only with propagation models which have vacuum path length distributions which do not differ greatly from exponential. The source abundances of nuclei withZ=15, 17, 18, 19, 21, 22, 23, 24, and 25 are found to be <0.02×Fe. For the remaining nuclei, Na, Al, S, and Ca are found to have source abundances of 0.07, 0.11, 0.18 and 0.13 of Fe respectively. The source abundance of C and O relative to Fe is also much different than some earlier compilations. A comparison of solar and cosmic ray abundances reveals certain selective differences, rather than a systematic overabundance of heavy nuclei in cosmic rays, as has been suggested in the past. These differences are discussed in terms of a common nucleosynthesis origin of the two species of particles.

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