Modification of the Symmetry Energy by Strangeness

Correct modeling, i.e. reproduction of global parameters as well as the internal structure of a neutron star requires specification of an equation of state of dense asymmetric nuclear matter. Different models describing matter of a neutron star have been developed. They are becoming more and more complex mainly due to the increase in the diversity of the chemical composition of this matter. At densities relevant for neutron star interiors, the exotic form of matter such as hyperons is expected to emerge. To get a reliable neutron star model, every opportunity to confront a theoretical model with experimental constraints is extremely valuable. The most important astrophysical constraint requires that theoretical models must lead to an equation of state that gives a maximum mass at least equal to the largest mass determined observationally, which is of the order of 2M [1, 2]. A very important aspect of theoretical modeling of a neutron star is the possibility of studying its internal structure, i.e. finding a solution for the radial distribution of particle numbers, isospin asymmetry or other quantities that characterize neutron star matter. This is currently beyond the experimental range. However, modification of the chemical composition of neutron star matter by including hyperons as additional degrees of freedom changes both