Equation of State of Hypernuclear Matter and Neutron Stars

  • A. Rios
  • A. Polls
  • A. Ramos
  • I. Vidaña
Part of the Lecture Notes in Physics book series (LNP, volume 652)


These lectures contain a pedagogical introduction to the equation of state of nuclear matter and to the structure of neutron stars. Particular attention is devoted to the β-equilibrium conditions and to the composition of neutron stars. The possible appearance of hyperons to reach the β–equilibrium when the density increases is carefully analyzed. In general, the introduction of new degrees of freedom, such as for instance the hyperons, produces a softening of the equation of state and as a consequence the maximum mass of the neutron star decreases. Finally, relevant observational data are compared with microscopic predictions.


Neutron Star Nuclear Matter Saturation Density Ladder Diagram Symmetric Nuclear Matter 
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Authors and Affiliations

  • A. Rios
    • 1
  • A. Polls
    • 1
  • A. Ramos
    • 1
  • I. Vidaña
    • 2
  1. 1.Departament d’Estructura i Constituents de la Matèria. Universitat de Barcelona, Diagonal 647, Barcelona 08028Spain
  2. 2.Gesellschaft für Schwerionenforschung (GSI), Planckstrasse 1, 64291 DarmstadtGermany

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