Charge Spectrum of the Heavy Primary Cosmic Rays

Citation

Stern, Edward Abraham (1955) Charge Spectrum of the Heavy Primary Cosmic Rays. Dissertation (Ph.D.), California Institute of Technology. doi:10.7907/JXAV-WY56. https://resolver.caltech.edu/CaltechETD:etd-01272004-152920

Abstract

NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. A measurement at [...] and 95,000 feet was made of the heavy primary cosmic-ray charge spectrum [...] by means of a pulse ionization chamber. The characteristics of the chamber and associated electronics are described. The effect of nuclear stars on the counting rate of the chamber was determined experimentally by sending up simultaneously two chambers, one filled with argon at half the pressure of the other. Slow evaporation particles will stop in the chambers and give the same pulses independent of pressure. Cosmic rays give pulses proportional to the gas pressure. Comparing the two chamber counting rates permits a determination of the star contribution. Other causes of the background counting rate were discussed and corrected for. It was concluded that Be and B combined are as abundant in the primary beam as the CNO group. The flux of the heavy particles [...] was also determined. It was not possible to obtain any information on the abundance of Li. A suggested improved version of the equipment is described and possible experiments are discussed.

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