[en] An examination is made of possible primary cosmic ray energy spectra which are consistent with observed air shower size spectra. At the size spectrum knee, it is necessary to have a very sharp primary spectrum break in order to be consistent with both the size spectrum and also air shower fluctuations. Such a break may be due to energy loss at the cosmic ray source

No abstract available

[en] It has recently been reported that cosmic ray showers arrive in an appreciably nonrandom manner with an excessive number of short time intervals between showers. The authors have investigated the distribution of time intervals between showers of size Nsub(e) approximately > 10⁵ and find that if there is any excess of short intervals it must be approximately < 5%

[en] Observations of cosmic ray air showers (median primary energy: 5.10¹³ eV) in Tasmania have been planned to start during 1981. The observations will be carried out through collaboration of the Hobart and Nagoya groups, in order to catch cosmic ray flows in a somewhat stereoscopic manner with simultaneous observations in the northern hemisphere (Mt. Norikura). The air shower array consists of 18 unit trays of 4 m² proportional counters deployed over an area of 20 m x 160 m. The shower frequency in a fundamental coincidence mode is expected to be about 16,000 events per hour

No abstract available

[en] Measurements have been made of the cosmic ray anisotropy at 35 deg S with a sea-level unshielded air shower array sensitive primarily to the proton component of the cosmic ray beam with energies between 10¹⁴ and 3 x10¹⁵eV. The first harmonic of the anisotropy was found to have an amplitude of 0.34(±0.09)% at a phase of 318(±18) deg. 13 refs., 1 fig

[en] The energy and mass composition of cosmic rays influence how the energy density of the radio emission of air showers is distributed on the ground. A precise description of the radio profiles can, therefore, be used to reconstruct the properties of the primary cosmic rays. Here, such a description is presented, using a separate treatment of the two radio-emission mechanisms, the geomagnetic effect and the charge excess effect. The model is parametrized as a function that depends only on the shower parameters, allowing for a precise reconstruction of the properties of the primary cosmic rays. This model is applied to cosmic-ray events measured with LOFAR and it is capable of reconstructing the properties of air showers correctly.

[en] An automaton is described for handling x-ray and other photographic film. The automaton performs stepped scanning of a rectangular sector of film having the dimensions approximately 410x500 μ. h scanning skp is 16+-1μ. A scanning step is 16+-1μ. During the scanning process photometry of the film is performed with a stipulated step plus output of the measurement results onto punched tape

[en] The measured cosmic ray energy spectrum exhibits clear structure (the knee) at approx 3 x 10 to the 15th power eV (sea level shower size approx 3 x 10 to the 5th power particles). Additionally, at energies in this general region, there occur apparent changes in shower development such that the observed characteristics of showers at this energy appear different to those characteristics observed at somewhat higher energies. At energies just below this region, the cosmic ray anisotropy amplitude apparently begins a progressive increase with energy. The latter effect does not clearly fit with the first two since there appears to be no significant change exactly at the knee. However, the phase of the first harmonic of the anisotropy appears to show a substantial change just where the energy spectrum shows structure and in the middle of the shower development changes. The first harmonic phase appears to change from approx. 18 hours R.A. to approx. 5 hours R.A. as the energy of observation moves through the knee. In this paper the latter change is examined in some detail by taking into account information contained in the second harmonic of the anisotropy

[en] The investigation is devoted to calculation of distribution of a fraction of full number of particles in a (maximum) detector for the thresholds N_c ≥ 170 and N_c ≥ 625 relativistic particles. The comparison with the experimental data is presented