Speaker
Description
We investigate the impact of dark matter on the structure and deformation of magnetars. We adopt a perturbative approach to model magnetic-field-induced deformation and assume that dark matter interacts with hadronic matter only through gravity. Under the assumption that dark matter is significantly softer than hadronic matter, we find that magnetic fields can indirectly influence the dark matter distribution via space–time deformation. We observe that the number of stars possessing a dark matter halo extending beyond the visible surface increases with both the dark matter fraction and the stiffness of the dark matter equation of state. As magnetic fields deform the star away from spherical symmetry, a non-symmetric dark matter halo can form outside the stellar surface. This deformation leads to discrepancies in the observed spin period P, its derivative P dot, and the emitted gravitational wave signals. The observed visible surfaces predict a lower period and gravitational wave strain than that with a dark matter halo. This can have interesting observational gravitational signatures unique to magnetars having a dark matter halo.