ALBERT

Notes: Abstract The integral flux of low energy protons (〉 10 MeV) observed by the University of New Hampshire cosmic ray detector aboard the Pioneer 9 spaceprobe has been compared with similar measurements of the near-Earth spacecraft Explorer 34 during the decay phase of the February 25–March 2, 1969 series of solar cosmic ray events. At this time the Pioneer 9 spaceprobe was 0.8 AU from the Sun and close to the Sun-Earth radial line. The ratio of integral fluxes as measured by the separated spacecraft can be calculated theoretically during the convective phase of the decay of these events and will depend on whether energy loss processes are operative. A comparison of the observed and theoretically calculated ratios suggests that the adiabatic energy loss process is operative.

Notes: Abstract A statistical analysis of solar particle events, observed by the GSFC-UNH charged particle detector on board Pioneer 10 and Pioneer 11 from March 1972 to December 1974 (from 1 to 5 AU for each spacecraft), is carried out with the goal of experimentally determining the statistical average interplanetary propagation conditions from 3 to 30 MeV. A numerical propagation model is developed that includes diffusion with a diffusion coefficient of the form k r =k o r β , convection, adiabatic deceleration, and a variable coronal injection profile. The statistical analysis is carried out by individually analyzing each of five parameters (t max, ξ(tmax), Δt 5, τ) that are uniquely defined in a solar particle event. Each of the five parameter data sets were analyzed in terms of both a spacecraft-solar flare connection longitude ≤50°, and a numerical model that employed a variable exponential decaying coronal injection profile. The five individual parameter analyses are combined with the results that the statistical average radial interplanetary diffusion coefficient from 1 to 5 AU is given by 〈k r〉 = (1.2 ± 0.4) × 1021 cm2 s-1 with 〈β〉 = 0.0± 0.3 for 3.4 to 5.2 MeV protons and 〈k r〉 = (2.6 ± 0.6) × 1021 cm2 s-1 with (β) = 0.0± 0.3 for 24 to 30 MeV protons. Using the classical relationship for the radial scattering mean free path λr, i.e. k r = υλr/3, we obtain 〈λr〉 = 0.09 ± 0.03 AU and 0.075 ± 0.020 AU for the low and high energy data, respectively. These results show, from 1 to 5 AU and from 3 to 30 MeV, that 〈λr〉 is both independent of radial distance and approximately independent of rigidity (for 〈λr〉~P α, where P = rigidity, α = -0.15 ± 0.20). The above diffusion coefficients are inconsistent With both the predictions of the diffusion coefficient from present theoretical transport models and with the diffusion coefficient used in modulation studies at low energies.

Notes: [Auszug] The radioactive isotope 26A1 has a half-life of 7.4xl05yr, decaying into an excited state of 26Mg 82% of the time by emission of a positron and 18% of the time by electron capture. 26Mg decays to its ground state 99.7% of the time by emission of a 1.81-MeV ?-ray. There is, therefore, a relationship ...

Notes: Abstract Stomach contents of 687 orange roughy [Hoplostethus atlanticus (Collett, 1889)] from the Challenger Plateau, sampled in March, July and November 1984, were examined. The relative importance of different components of the diet was assessed using three feeding indices which combine, in different ways, percentage frequency of occurrence, percentage number, and percentage weight of prey categories. For both sexes, for all size classes and at any time of the year, the most frequent and abundant components of the diet were prawns, followed by fish, squid, amphipods and mysids. The main natant decapod families were Oplophoridae, Pasiphaeidae, and Sergestidae. Fish, mainly Chauliodontidae and Myctophidae, were the most important prey by weight. Most prey species were benthopelagic and mesopelagic organisms which move towards the surface at night. However, H. atlanticus can be caught by bottom trawl (between 750 and 1 200 m) during any 24 h period, and there was no evidence of vertical migration in search of their prey. When the fish grow in length, there is a transition in the diet from prawns, mysids, and fish, to prawns, fish and squid. Squid were not found in the stomach contents of fish smaller than 20 cm. These dietary changes may be linked to modifications in morphology with growth. The relative proportions of the main dietary items, and in particular the natant decapod families, varied with time of the year. Also, the stomach data seem to indicate an increasing importance of fish and squid in the diet in deeper water. H. atlanticus appears to be an opportunistic predator, consuming a wide variety of invertebrates and fishes. Our results provide evidence to support the notion that benthopelagic predators which consume vertically migrating mesopelagic fish, have an important role in the transfer of energy to the benthos.

Notes: Abstract Using a balloon borne double dE/dx x total energy telescope we have determined the isotopic composition of cosmic ray Li, Be and B nuclei in the energy range 100–250 MeV nuc.−1. The measured mass resolution, σ for these nuclei is ∼0.3 AMU. The observed isotopic composition is in agreement with that predicted on the basis of interstellar fragmentation with the exception of a deficiency of Be10. If the low abundance of Be10 is attributed to the decay of this radioactive isotope we obtain a mean cosmic ray lifetime of (3.4 −1.3 +3.4 )×106 yr.

Notes: Abstract We report on new measurements of the spectra of Li, Be and B nuclei in the primary cosmic radiation in the energy range 100 MeV/nuc to 〉22 BeV/nuc. The differential spectrum of these light nuclei is found to have a maximum at ∼400 MeV/nuc in 1966. The L/M ratio is found to be equal to 0.25±0.01, constant over the entire energy range of the measurement. Atmospheric and solar modulation effects on the L nuclei and the L/M ratio are discussed. It is concluded that this ratio is representative of conditions in interstellar space. Using the most recently available fragmentation parameters gives a material path length of 3.6 g/cm2 of hydrogen for the particles producing the L nuclei. The absence of any variation of the L/M ratio with energy places severe constraints on models for the propagation of cosmic rays. Models in which the material path length is a strong function of energy — or that exhibit an exponential path-length distribution for a fixed energy are incompatible with these results. An examination of the abundance ratios of the individual L nuclei separately reveals major discrepancies with the predictions of interstellar diffusion theory based on presently accepted fragmentation parameters. The constancy of the measured Li/M and B/M ratios with energy is not in accord with the large energy dependence of these ratios expected from the energy dependence of the fragmentation cross-sections. The low Li/M ratio and high B/M ratio to be expected if these nuclei are created at a much lower energy than we observe are also not found. This presents difficulties for theories which suggest that the passage through matter has occurred at low energies subsequently followed by considerable acceleration. The Be/M ratio in cosmic rays is anomalous in that it is ∼40% larger than expected on the basis of the fragmentation cross-sections. Evidence presented here on the isotopic composition of Be nuclei suggests that this discrepancy is due to an enhanced abundance of Be9 or Be10 in cosmic rays. This discrepancy complicates the determination of a cosmic-ray ‘age’ using the decay of Be10 into B. Nevertheless the Be/B ratio is observed to remain constant at 0.42±0.03 over the energy range from 100 MeV/nuc to over 10 BeV/nuc. Unless the fragmentation parameters into the various isotopes of Be and B are such that e.g. Δ(Be/B)〈0.05 as a result of this decay, then the age of cosmic rays is either 〉3×108 years or 〈106 years. The further observation that the mass to charge ratio of all Be nuclei of energy ∼1 BeV/nuc is =2.05±0.1 suggests that Be10 is present at these energies. This supports the idea of a short lifetime.

Notes: Abstract From our recent observations of the charge and energy spectra of cosmic-ray nuclei we have constructed secondary-to-primary charge ratios at the two ends of the charge spectrum. These ratios are found to be inconsistent with thead hoc leaky-box model of cosmic-ray propagation which leads to an exponential pathlength distribution. Models for which the pathlength distribution function is deficient in short pathlengths provide a more consistent picture. Several of these models are investigated, bothad hoc and physical. The physical model considered here is one for which detailed galactic propagation parameters and boundary conditions are used and for which there exists no near sources of cosmic rays over a time interval corresponding to a few times the cosmic-ray age.

Notes: Abstract Measurements of the energy spectra of carbon and oxygen nuclei in the primary cosmic radiation over the energy range from 140 MeV/nuc to 30 BeV/nuc are reported. An average C/O ratio of 1.11±0.02 is obtained at the top of the atmosphere. This ratio is found to be constant to within ∼5% over the entire energy range. The energy spectra of these two nuclei are presented and compared with earlier measurements and with satellite observations at low energies. After correction for propagational effects in 4 g/cm2 of interstellar hydrogen the ‘source’ C/O ratio is found to be ∼0.9. The astrophysical implications of this C/O ratio are discussed.

Notes: Abstract This paper summarizes new data in several fields of astronomy that relate to the origin and acceleration of cosmic rays in our galaxy and similar nearby galaxies. Data from radio astronomy shows that supernova remnants, both in our galaxy and neighboring galaxies, appear to be the sources of most of the accelerated electrons observed in these galaxies. γ-ray measurements also reveal several strong sources associated with supernova remnants in our galaxy. These sources have γ-ray spectra that are suggestive of the acceleration of cosmic-ray nuclei. Cosmic-ray observations from the Voyager and Ulysses spacecraft suggest a source composition that is very similar to the solar composition but with distinctive differences in the 4He, 12C,14 N and 22Ne abundances that are the imprint of giant W-R star nucleosynthesis. Injection effects which depend on the first ionization potential (FIP) of the elements involved are also observed, in a manner similar to the fractionization observed between the solar photosphere and corona and also analogous to the preferential acceleration observed for high FIP elements at the heliospheric solar wind termination shock. Most of the 59Ni produced in the nucleosynthesis of Fe peak nuclei just prior to a SN explosion appears to have decayed to 59Co before the cosmic rays have been accelerated, suggesting that the59 Ni is accelerated at least 105 yr after it is produced. The decay of certain K capture isotopes produced during cosmic-ray propagation has also been observed for the first time. These measurements suggest that re-acceleration after an initial principal acceleration cannot be large. The high energy spectral indices of cosmic-ray nuclei show a significant charge dependent trend with the index of hydrogen being -2.76 and that of Fe -2.61. The escape length dependence of cosmic rays from our galaxy can now be measured up to ~300 GeV nucl-1 using the Fe sec/Fe ratio. This escape length is ∼P -0.05 above 10 GeV nucl-1 leading to a typical source spectral index of (2.70±0.10) -0.50 = -2.20 for nuclei. This is similar to the source index of -2.3 inferred for electrons within the errors of ±0.1 in the index for both components. Spacecraft measurements in the outer heliosphere suggest that the local cosmic-ray energy density is ~2eV cm-3 – larger than previously assumed. Gamma-ray measurements of electron bremsstrahlung below 50 MeV from the Comptel experiment on CGRO show that fully 20–30% of this energy is in electrons, several times that previously assumed. New estimates of the amount of matter traversed by cosmic rays using measurements of the B/C ratio are also higher than earlier estimates – this value is now ~10 g cm-2 at 1 GeV nucl-1. Thus altogether cosmic rays are energetically a more important component of our galaxy than previously assumed. This has implications both for the types of sources that are capable of accelerating cosmic rays and also for the role that cosmic rays may play in ionizing the diffuse interstellar medium.

Notes: Abstract A recently reported measurement of a small electron gradient in the energy range 1.9–8.4 MeV by Webber et al. (1973a) is interpreted in terms of a large local value of the scattering mean free path for these particles. The possibility that the scattering mean free path may be large throughout the modulation region is then investigated under the assumption of an azimuthally symmetric modulation region of 5 AU extent, the applicability of the diffusion-convection-adiabatic energy loss transport equation, and a galactic origin for the low energy electrons. The implications for the solar modulation of electrons and the interstellar electron spectrum are discussed.