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Structure and stability of adiabatic fluid spheres using a scalar theory of gravitation. Lee, Clinton Arthur

Abstract

A scalar theory of gravitation is used to construct stellar models which are static, spherically symmetric, isentropic, and composed of an ideal fluid obeying a power-law pressure-density relation. Such a relation holds for an isentropic non-degenerate perfect gas and for a degenerate Fermi gas In which the particles are non-relativistic or ultra-relativistic. A method for determining if a given static, spherically symmetric configuration is unstable against radial adiabatic perturbations is derived for the scalar theory. It is specialized to the particular models constructed. Numerical results on the structure and stability of the models are obtained and compared with general relativistic results. It Is found that the static results agree qualitatively with those given by general relativity but disagree quantitatively, e.g., a larger maximum mass for neutron stars is found using the scalar theory. The dynamical results are found to differ with those given in general relativity.

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