[en] In general a particle transport model for energetic solar flare particles contains a number of free parameters which are determined by fitting various features of observed particle events. Frequently the parameter values are not uniquely determined. In order to place tighter constraints on the models, the anisotropy of 1 and 25 MeV/nuc protons and helium nuclei were examined during the 22 November 1977 solar particle event using data from the LECP experiment on Voyager 1 at 1.6 AU. These observations were combined with the time intensity profiles at Voyager 1 and at 1 AU from ISEE-1 and IMP-8 to determine the magnitude and radial dependence of the interplanetary diffusion coefficient and the required injection duration at the sun. The first order anisotropy amplitudes for both 1 MeV and 25 MeV protons are observed to decrease from maximum values (approx. 1) during the event onset at Voyager 1 to values consistent with convection in the solar wind at about 3 days into the event decay phase. The intensity and anisotropy profiles at 1.6 AU are consistent with predictions of diffusive transport with a modest mean free path (lambda = approx. 0.1 AU). 1 reference

[en] We have surveyed the temporal variations of the relative abundances of 0.6--2.4 MeV per nucleon ions accelerated in solar particle events whose parent flares were located in the so-called well-connected region between W20⁰ and W80⁰ solar longitude. The survey was carried out under solar minimum conditions from 1973 November to 1977 December using the University of Maryland/Max-Planck-Institut ULET telescope on the IMP 8 spacecraft. Several particle events were found which originated in the well-connected region, and of these, two events appeared remarkably free of contamination from other solar particle events or interplanetary disturbances. During the rise phase, the abundances measured at 1 AU were characterized by large (factor of approx.5) decreases in the Fe/O ratios, of the type reported by others, as well as significant decreases in the O/He ratio. After examination of several mechanisms which might cause the abundance variations, it is concluded that the rise phase variations may be understood in terms of interplanetary propagation effects. A detailed comparison of model calculations with the rise phase observations leads to the conclusion that the radial interplanetary scattering mean-free-path varies with rigidity as lambda_rproportionalP^{0.61plus-or-minus0.18}, in agreement with calculations from the quasi-linear theory. However, the size of lambda_r approx.0.1--0.2 AU is larger than predicted by the theory

[en] Energetic particle flux enhancements over the period October 1973 - December 1977 were surveyed using ULET sensor on the IMP-8 spacecraft. During the four year period the most extreme periods of Fe enrichment compared to oxygen were during solar flare events in February 1974 and May 1974. In these same events, the carbon abundance with respect to oxygen was significantly depleted when compared with a value C:O approximately = 0.45:1 for typical solar flares. These observations, taken together with previously reported 3-He enrichment in these events, give strong evidence for the importance of a wave-particle interaction in the pre-injection heating of the ambient matter

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[en] A survey of the approx. 1 MeV/nucleon heavy ion abundances in 66 He³-rich solar particle events was performed using the Max-Planck-Institut/University of Maryland and Goddard Space Flight Center instruments on the ISEE-3 spacecraft. The observations were carried out in interplanetary space over the period 1978 October through 1982 June. Earlier observations were confirmed which show an enrichment of heavy ions in HE3-rich events, relative to the average solar energetic particle composition in large particle events. For the survey near 1.5 MeV/nucleon the enrichments compared to large solar particle events are approximately He4:C:O:Ne:Mg:Si:Fe = 0.44:0.66:1.:3.4:3.5:4.1:9.6. Surprising new results emerging from the present broad survey are that the heavy ion enrichment pattern is the same within a factor of approx. 2 for almost all cases, and the degree of heavy ion enrichment is uncorrelated with the He³ enrichment. Overall, the features established appear to be best explained by an acceleration mechanism in which the He³ enrichment process is not responsible for the heavy ion enrichment, but rather the heavy ion enrichment is a measure of the ambient coronal composition at the sites where the He³-rich events occur

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[en] Fourteen transverse, nearly vertical, successive faces were excavated, surveyed, sampled, and photographed to document the characteristics of the test burn cavity produced by the 1983 CRIP experiment. The cavity area exhibited a basically flat-bottomed and vertical-walled geometry. The reaction zone along the bottom and side walls was less than six inches in thickness. Samples taken were analyzed by proximate, elemental, and X-ray diffraction techniques. Results presented here indicate a steep temperature gradient across the reaction wall and temperatures in excess of 1200⁰C in altered overburden material. The sequence of mineralogic changes with increasing temperature is qualitatively identified

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