Towards a ‘just’ conservation psychology

Climate change and biodiversity loss are serious concerns for environmental researchers and conservationists. However, the impact of climate change and biodiversity loss disproportionately affects low-income communities, indigenous groups, and people of colour. Conservation initiatives, however, sometimes perpetuate historical injustices of marginalised people. We argue that environmental justice may be effectively merged with conservation psychology to promote a just conservation psychology. We discuss a case study of a South African community impacted by conservation-related environmental injustices under apartheid. We discuss the role of capacity building in a community-based conservation initiative that promotes justice, human wellbeing, and conservation goals

The origin and propagation of VVH primary cosmic ray particles

Several source spectra were constructed from combinations of 4- and s-process nuclei to match the observed charge spectrum of VVH particles. Their propagation was then followed, allowing for interactions and decay, and comparisons were made between the calculated near-earth spectra and those observed during high altitude balloon flights. None of the models gave good agreement with observations

Primary cosmic ray particles with z 35 (VVH particles)

Large areas of nuclear emulsions and plastic detectors were exposed to the primary cosmic radiation during high altitude balloon flights. From the analysis of 141 particle tracks recorded during a total exposure of 1.3 x 10 to the 7th power sq m ster.sec., a charge spectrum of the VVH particles has been derived

The Isotopic Composition of Cosmic Ray Nuclei Beyond the Iron Peak

Isotope measurements of cosmic ray nuclei beyond the Fe peak are considered, using the charge region from Z=29 to Z∼40 as an example. Such studies can address a number of important questions that bear on cosmic ray origin, acceleration, and propagation. One possible approach for measuring isotopes with Z≥30 is based on large‐area arrays of silicon solid state detectors combined with scintillating optical fiber trajectory detectors optical fiber trajectory detectors

Energy spectra of elements with 18 or = Z or = 28 between 10 and 300 GeV/amu

The HEAO-3 Heavy Nuclei Experiment is composed of ionization chambers above and below a plastic Cerenkov counter. The energy dependence of the abundances of elements with atomic number, Z, between 18 and 28 at very high energies where they are rare and thus need the large area x time are measured. The measurements of the Danish-French HEAO-3 experiment (Englemann,, et al., 1983) are extended to higher energies, using the relativistic rise of ionization signal as a measure of energy. Source abundances for Ar and Ca were determined

Constraints on cosmic-ray acceleration and transport from isotope observations

Observations from the Cosmic Ray Isotope Spectrometer (CRIS) on ACE have been used to derive constraints on the locations, physical conditions, and time scales for cosmic-ray acceleration and transport. The isotopic composition of Fe, Co, and Ni is very similar to that of solar system material, indicating that cosmic rays contain contributions from supernovae of both Type II and Type Ia. The electron-capture primary ^(59)Ni produced in supernovae has decayed, demonstrating that a time ≳10^5 yr elapses before acceleration of the bulk of the cosmic rays and showing that most of the accelerated material is derived from old stellar or interstellar material rather than from fresh supernova ejecta

Interactions of heavy nuclei, Kr, Xe and Ho, in light targets

Over the past few years, the HEAO-3 measurements of the abundances of ultra-heavy cosmic ray nuclei (Z 26) at earth have been analyzed. In order to interpret these abundances in terms of a source composition, allowance must be made for the propagation of the nuclei in the interstellar medium. Vital to any calculation of the propagation is a knowlege of the total and partial interaction cross sections for these heavy nuclei on hydrogen. Until recently, data on such reactions have been scarce. However, now that relativistic heavy ion beams are available at the LBL Bevalac, some of the cross sections of interest can be measured at energies close to those of the cosmic ray nuclei being observed. During a recent calibration at the Bevalac of an array similar to the HEAO-C3 UH-nuclei detector, targets of raphite (C), polyethylene (CH2), and aluminum were exposed to five heavy ion beams ranging in charge (Z) from 36 to 92. Total and partial charge changing cross sections for the various beam nuclei on hydrogen can be determined from the measured cross sections on C and CH2, and will be applied to the propagation problem. The cross sections on Al can be used to correct the abundances of UH cosmic rays observed in the HEAO C-3 detector for interactions in the detector itself

Cosmic Ray Elemental Abundances for 26<Z<40 Measured on HEAO-3

Abundances relative to _(96)Fe have been derived for elements with charge, 2, in the range 32≤z≤40. With a resolution better than 0.5 charge unit at Z=38, we resolve _(37)Rb from _(38)Sr and use the Rb/Sr ratio to place a limit on the r-proccss enhancement of the cosmic ray source material in this charge range

The Abundances of the Heavier Elements in the Cosmic Radiation

We review current work on the abundances of the ultraheavy elements in the cosmic radiation, those with Z≳30. Those abundances are compared with predictions based on propagation and fractionation of elemental abundances from various assumed sources of the cosmic rays. We find striking similarities between the solar system and the cosmic ray source abundances for those elements with 32≤Z≤60. For elements with Z≳60, there appears to be a substantial enhancement in the abundances of elements synthesized in the r‐process