Interplay between hyperons and antikaons in E-RMF description of neutron stars

In the core of Neutron star (NS), the density is generally considered as high as several times the nuclear saturation density. At such high density, the conventional view of the NS, composed of nucleons and leptons, is insufficient and more realistic approaches are needed. With increasing density, the chemical potential of baryon and electric charge increases rapidly and they provide energy for the production of low energy hyperons and kaons. This effects in softening the EoS and hence reduce the maximum mass of NS. Hyperons can also influence transport properties and thermal evolution of the stars. The onset of kaon condensation could send neutron stars into low-mass black holes and hence it is very interesting issue to investigate the stability of NS with the inclusion of kaon condensation. Considering the fact that K− meson is more favoured at lower density than other kaon species, the study has taken only K− into account here. With a similar reason, the study chooses hyperon. With the inclusion of both K− and Λ the properties of NS matter is studied