Nuclear Structure Calculations for Astrophysical Applications PDF Download

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Languages : en
Pages : 12

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Book Description
Relative to other fields of physics, astrophysics is probably unique in its requirement that a very large number of physical environments be modeled to achieve a satisfactory description of the phenomena under study. The dynamics of the cosmos is governed by interactions that span a vast range, from subnucleon, nucleon and nuclear distances to distances affected by the gravitational interactions, which extends over the width of a galaxy and beyond, to the edge of the universe. It is the nuclear processes that provide much of the energy that drives the macroscopic behavior of the cosmos. Through this energy release the behavior on the very small scale is coupled to the very large-scale behavior. On the nuclear level, cross sections, nuclear decay energies and nuclear decay paths are but a few examples of quantities that are of paramount importance in astrophysical models. Because nuclei of extreme composition, quite different from what can be studied on earth, exist in stellar environments, an understanding of the nuclear structure properties of these nuclei can only be obtained through theoretical means. This presents a continuing, stimulating challenge to the nuclear-physics community. Here we present calculated results on such diverse properties as nuclear energy levels, ground-state masses and shapes, [beta]-decay properties and fission-barrier heights. Our approach to these calculations is to use a unified theoretical framework within which the above properties can all be studied. The results are obtained in the macroscopic-microscopic approach in which a microscopic nuclear-structure single-particle model with extensions is combined with a macroscopic model, such as the liquid-drop model.