Abstract
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.
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Rios, A., Polls, A., Ramos, A., Vidaña, I. Equation of State of Hypernuclear Matter and Neutron Stars. In: Arias, J.M., Lozano, M. (eds) The Hispalensis Lectures on Nuclear Physics Vol. 2. Lecture Notes in Physics, vol 652. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-44504-3_8
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DOI: https://doi.org/10.1007/978-3-540-44504-3_8
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