Antikaon condensation in magnetized neutron stars

Abstract

This study investigates the possibility of antikaon condensation in strongly magnetized neutron stars (NSs) with [Formula: see text]-equilibrium condition using chiral [Formula: see text] model and chiral perturbation theory (ChPT). We explore the effect of finite strong magnetic field on particle fraction, effective masses of kaon/antikaon, and equation of state (EoS). The longitudinal EoS gets softened; whereas in transverse EoS, stiffness is observed as the magnetic field strength increases. The presence of antikaon condensation causes softness in both the longitudinal and transverse EoS. Finally, we investigate the structure of NSs through the mass–radius relation, tidal deformability, and Love number and present possible comparison with recent work in the field. The presence of antikaon condensed phase decreases the mass of NSs corresponding to both EoS (longitudinal and transverse). For longitudinal pressure, the mass–radius shows decrement with increase in magnetic field strength; whereas transverse pressure causes an increment.