Ultra-heavy cosmic rays: Theoretical implications of recent observations

Extreme ultraheavy cosmic ray observations (Z greater or equal 70) are compared with r-process models. A detailed cosmic ray propagation calculation is used to transform the calculated source distributions to those observed at the earth. The r-process production abundances are calculated using different mass formulae and beta-rate formulae; an empirical estimate based on the observed solar system abundances is used also. There is the continued strong indication of an r-process dominance in the extreme ultra-heavy cosmic rays. However it is shown that the observed high actinide/Pt ratio in the cosmic rays cannot be fit with the same r-process calculation which also fits the solar system material. This result suggests that the cosmic rays probably undergo some preferential acceleration in addition to the apparent general enrichment in heavy (r-process) material. As estimate also is made of the expected relative abundance of superheavy elements in the cosmic rays if the anomalous heavy xenon in carbonaceous chondrites is due to a fissioning superheavy element

On the e-Process: Its Components and their Neutron Excesses

The pattern of abundances within the iron-abundance peak of the solar system is analyzed for various Cr, Fe, and Ni abundances, and a method is developed for finding the best fit to a given set of abundances with a chosen number of zones, i.e., mass contributions characterized by differing values of eta. This material can be synthesized by a superposition of e-process compositions in a low-eta region (eta = 0.003) and a high-eta region (eta = 0.065 -0.080) with at least 85% coming from the low-eta region. Addition of a third eta zone is unproductive. The applicability of the particle-poor freeze out is discussed in the light of these abundances, and the results of employing different numbers and types of zones are interpreted as an indication of the relative abundances themselves. Ejection of the low-eta zones is of great interest in gamma-ray astronomy and for empirical testing of theories of nucleosynthesis. The distribution of high zones should give important information about the formation of collapsed remnants

Biblisches Spruchbuch zum Religionsunterricht in israelitischen Schulen

von L. M. Hainebac

Nuclear statistical equilibrium and the iron peak

The equations governing the abundance distribution of the nuclear species (atomic nuclei) under conditions of statistical equilibrium of the strong nuclear interaction are rederived and discussed. An algorithm for their solution on a computer is presented, giving abundance distributions as a function of temperature, density and overall neutron-proton ratio. A computer search of nuclear species abundance distributions and mixtures of two distributions is carried out in an attempt to match equilibrium distributions, after weak interaction decay, of certain "iron peak" species to their observed solar system distributions. A mixture is found which reproduces the solar system abundance distribution of Fe 54,56,57,58. Ninety-nine percent of the Fe56 is produced in nuclear statistical equilibrium as Ni56, lending hope to the proposed observation by gamma ray astronomy of the decay of Ni56 to Fe56 following a supernova event

Cross Language Retrieval - English / Russian / French

This paper brings together discussions of three distinct lines of research, each of which has resulted in a working software product for the database production environment: machine aided indexing, a state-of-the-art translation system, and a multilingual search and retrieval system and interface. 1) The MAI - Machine Aided Indexing software developed by Access Innovations