[en] Differential spectra of even charged nuclei between Si and Fe in the August 4, 1972 event were made in the energy region of 10 to 40 MeV/n-1 using rocket borne plastic detectors. The resulting relative abundances of elements and low energy enhancements are obtained and compared with spectroscopically determined photospheric abundances. The implications of the relative abundances on the acceleration mechanisms is discussed

[en] In the Indian cosmic ray experiment (IONS) in Spacelab-3 the intention is to study nuclei up to iron in low energy cosmic rays, using CR-39 (DOP) detectors. CR-39 (DOP) was exposed to He-4, C-12, O-16, Ne-20, Si-28, Ar-40, Cr-52 and Fe-56 accelerated beams from various accelerator facilities available around the world. Different beam energies and exposure angles were used. From these exposures, the charge resolution and energy resolution for the detector in the region of interest were studied. The effect of pre-annealing and depth on the response of our detector was studied. For isotopic resolution, the detector samples were exposed to Ne-2O and Ne-22 accelerated beams. Samples of CR-39 (DOP) exposed to different accelerated heavy ions were kept in the detector module to take into account the effect of ambient conditions on detector response during the flight

[en] Analysis of data regarding the particles that are emitted in particle flares for the last 25 years makes it possible to identify some of the common features of solar particle emission which should be explained theoretically. It appears that the flares must be divided into large and small flares depending on the energetics and the fluxed emitted in these events. In large events it is also possible to suggest (from the fact that C, N, O, Ne, S, and Ar are never enhanced in flares) that the temperature of the plasma from which these particles are emitted must be 3 x 10 to the 6th K for all flares. The observations are a good indication regarding conditions in the particle-emitting regions of the sun. 33 references

[en] A Lexan polycarbonate detector exposed on the exterior of Skylab-3 for 73 days during a solar quiet period was used to study the relative abundances of calcium to nickel ions in low energy cosmic rays of 50 to 250 MeV/N. The method of charge identification is based on the measurement of conelength (L) and residual range (R) of these particles in various Lexan sheets. Since more than one cone (sometimes as many as five) is observed and is measured, the charge accuracy becomes precise and accurate. The ratio of (calcium to manganese) to (iron and cobalt) obtained at three energy intervals of 50 to 80, 80 to 150, 150 to 250 and 50 to 250 MeV/N are 7.6 plus or minus 3.8, 2.7 plus or minus 0.8, 1.4 plus or minus 0.6 and 3.3 plus or minus 0.7 respectively. These data thus indicate a large increase of this ratio with decreasing energy. The origin of this strong energy dependence is not understood at present

[en] The origin and the ionization states of the anomalous component of the cosmic ray nuclei in the energy region 1-30 MeV/amu recently observed in interplanetary space are investigated in detail. It was assumed that this component originated from nearby sources, e.g. from novae type explosions (which have peculiar C, N and O compositions) and are further accelerated in the interplanetary medium. Modulation of these ions is also calculated and a comparison is made of the demodulated composition of C-Si ions with the available abundance data of some novae. (author)

[en] The progress is presented of the nuclear emulsion experiment to determine abundance of low energy antiprotons in cosmic rays. No antiprotons have been detected so far at upper limit of p/p less than or similar to 4 x .0001 in the energy range 50 MeV to 15 MeV

[en] The origin of the new component of cosmic ray nuclei in 1-30 MeV amu^-1 recently detected through space vehicles in interplanetary space is investigated in detail. It is assumed that these particles may originate from nearby sources, e.g., from novae type explosions, which have peculiar C, N and O compositions. These particles are further assumed to be accelerated and modulated within the heliosphere. The charged states of these ions in the interstellar space have been calculated in detail and it is shown that the same charged states are preserved in the heliosphere when they are accelerated to energies of the order of 10⁷ eV amu^-1 from energies of > approximately 10⁵ eV amu^-1. Modulation of these ions are calculated and it is found that because of low charged states of the ions these have high rigidities and are modulated in such a way as to enhance the O-ion abundances as compared to C-ions. A comparison is made of the demodulated composition of C to Si-ions with available abundance data of some novae. (Auth.)

[en] The study of cosmic-ray heavy ions (Z = 6-28) at 1-100 TeV/n can provide important clues to cosmic-ray origin and propagation in interstellar space. Characteristics of high-energy particle interaction beyond the accessible range of present-day accelerators could also be obtained. A preliminary outline of a detector system for such an experiment, which can be carried out on the proposed Space Station, is presented. It consists mainly of CR-39 and emulsion detectors interspaced with thin copper targets to facilitate fragmentation of the incident CR heavy ions. Charge resolution of Delta-Z = 0.2 can be obtained with the CR-39 plastic detector, and the opening angle of collision fragments traced in nuclear emulsions can be used to determine the particle energies. Time resolution of about 30 sec for the arrival of the relativistic particles can be achieved. The details of the proposal are discussed

[en] The possible origin of the anomalous cosmic rays (ACR) are studied in terms of stellar wind injection from O type stars and their acceleration in shock fronts of SNR's. It is assumed that a fraction of heavy ions will encounter interstellar shock fronts of SNR's and these are accelerated to about 5 to 100 MeV/N and give rise to ACR's. Typically these ions would travel a distance of the order of a few 1000 pc. Therefore it is estimated that O type stars in a volume of radius of a few Kpc around the solar system are contributing to the intensity of ACR in the local ISM. From observational data, the intensity of ACR in the local ISM is estimated. It is suggested that these ACR ions enter the solar system along the solar dipole field lines connected to the interplanetary magnetic field lines

[en] Recent observations in space vehicles have indicated an increase in the intensity of the cosmic ray nuclei below 30 MeV/amu in interplanetary space. The charged states of these ions are calculated by assuming that these particles come from nearby sources having energies around 10⁵ ev/amu. If further accelerated to 10⁷ ev/amu in interplanetary medium, they could possibly account for this new component. (author)