Microscopic Theory of the Nuclear Equation of State and Neutron Star Structure

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dc.creatorBaldo, Marcello
dc.creatorBurgio, Fiorella
dc.date2000-12-05
dc.date.accessioned2026-07-07T05:38:23Z
dc.date.available2026-07-07T05:38:23Z
dc.descriptionThe Bethe-Brueckner-Goldstone many-body theory of the Nuclear Equation of State is reviewed in some details. In the theory, one performs an expansion in terms of the Brueckner two-body scattering matrix and an ordering of the corresponding many-body diagrams according to the number of their hole-lines. Recent results are reported, both for symmetric and for pure neutron matter, based on realistic two-nucleon interactions. It is shown that there is strong evidence of convergence in the expansion. Once three-body forces are introduced, the phenomenological saturation point is reproduced and the theory is applied to the study of neutron star properties. One finds that in the interior of neutron stars the onset of hyperons strongly softens the Nuclear Equation of State. As a consequence, the maximum mass of neutron stars turns out to be at the lower limit of the present phenomenological observation.
dc.description30 pages, 21 postscript figures included. Lecture presented at the workshop on "Physics of Neutron Stars Interior" held at the European Center for Theoretical Nuclear Physics, June 2000, Trento, Italy. To be published in Lecture Notes in Physics, eds. D. Blaschke, N. K. Glendenning and A. Sedrakian (Springer, 2001)
dc.identifierhttps://arxiv.org/abs/nucl-th/0012014
dc.identifierhttp://arxiv.org/abs/nucl-th/0012014
dc.identifierLect.Notes Phys. 578 (2001) 1-29
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/81596
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleMicroscopic Theory of the Nuclear Equation of State and Neutron Star Structure
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