Abstract
I review the issues related to the appearance of hyperons in neutron star matter, focusing in particular on the problem of the maximum mass supported by hyperonic equations of state. I discuss the general mechanism that leads to the formation of hyperons in the core of neutron stars and I review the main techniques and many-body methods used to construct an appropriate equation of state to describe the strongly interacting system of hadrons hosted in the core of neutron stars. I outline the consequences on the structure and internal composition of neutron stars and also discuss the possible signatures of the presence of hyperons in astrophysical dynamical systems like supernova explosions and binary neutron star mergers. Finally, I briefly report about the possible important role played by hyperons in the transport properties of neutron star matter and on the consequences of neutron star cooling and gravitational wave instabilities induced by the presence of hyperons.
Highlights
The birth of hyperon physics dates back to 1947 when Rochester and Butler observed the first hyperon by studying cosmic rays in a gas chamber [1]
In Ref. [202], Djapo and collaborators reported several BHF calculations based on a large variety of NY interactions provided by the Nijmegen (NSC89, Nijmegen Soft Core 1997 (NSC97)) and Jülich (Ju89, Ju04) groups supplemented by a phenomenological three-nucleon force, and using the Vlow−k technique to reduce the high-momentum component of the baryon-baryon interaction
The baryonic mass of the neutron star with a good approximation remains constant along the neutron star evolution and, it can be considered as an independent variable
Summary
The birth of hyperon physics dates back to 1947 when Rochester and Butler observed the first hyperon by studying cosmic rays in a gas chamber [1]. The huge density variation in the range ∼(1 − 1015) g/cm expected in neutron stars requires the modelling of systems in very different physical conditions, like heavy neutron-rich nuclei arranged to form a lattice structure, as in the outer crust of the star, or a neutral charge system of interacting hadrons and leptons forming a quantum fluid, as in the stellar core [11]. The description of such a variety of systems, of considerable interest for nuclear physics as well as for astrophysics, needs a challenging theoretical effort and an accurate knowledge of the interactions between the particles present inside the star. In the last part of this review, I report the possible signatures of the appearance of hyperons in astrophysical systems like BNSMs and SNe, as well as some possible important roles played by the presence of hyperons in hot young neutron stars
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