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An attempt has been made to determine the abundance of low-energy tritons and deuterons in a nuclear emulsion stack exposed at a geomagnetic latitude, λ =61° N on August 3, 1958 under 3.8 g/cm2 of matter. The grain density versus range method has been used for identification of the tracks produced by the singly charged nuclei. The selection criteria allow the observation of deuterons of kinetic energy (92÷175) MeV per nucleon and tritons of (73÷165) MeV per nucleon. The upper limits for the differential fluxes for tritons and deuterons are 3.5·10-3 and 9.2·10-3 peters per MeV for the energy ranges given above. The upper limit for the triton to α-particle ratio for the same rigidity (1.14 to 1.48 G-V) is 0.09. Some of the implications of these results are discussed. However, due to the uncertainty of the correction for secondary production within the atmosphere, the results are consistent with the absence of these elements in primary cosmic radiation |
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