  Dark matter remains a topic of ongoing controversy. It has gained attention
in the theoretical description of compact objects such as neutron stars with
cores of very dense matter. Various candidates have been proposed for dark
matter in the scientific literature. Among them, the sexaquark has been
identified as a potential bosonic particle capable of being formed in neutron
star matter based on its mass characteristics. In this study, we investigate
the viability of the sexaquark as a candidate for dark matter, particularly
under certain density conditions. Our goal is to address the challenges
associated with the formation of a bosonic particle in a highly dense medium
without compromising the stability of the neutron star. To achieve this, we
introduce a straightforward linear mass shift for the sexaquark within the
hadronic equation of state, utilizing a relativistic density functional
approach. In our investigation, it is observed that the inclusion of Sexaquark
as a candidate for dark matter within the hadronic matter equation of state,
although featuring a repulsive interaction with baryonic matter, softens the
equation of state. We suppose that the strength of the interaction of dark
matter with baryonic matter increases linearly with the baryon density. We
observe that raising the effective mass of the Sexaquark, as a result of
increasing its vacuum mass, causes an increased stiffening of the equation of
state as compared to the case of a constant mass. We determine the lower and
upper mass boundaries for this bosonic dark matter based on observational
constraints for neutron stars within the DD2Y-T model when a phase transition
to quark matter phase is employed.
