Speaker
Description
The impact of dark matter (DM) on highly magnetized neutron stars (NSs) is explored using a two-fluid approach. Our model considers self-interacting, non-annihilating, asymmetric fermionic DM coupled to baryonic matter via gravity. Using the relativistic mean-field model with density-dependent magnetic fields, we examine how DM particle mass, mass fraction, and magnetic field strength affect the NS equation of state, structure, and stability. Our analysis shows that increasing the DM fraction reduces the maximum gravitational mass of NSs, especially for heavier DM particles. In contrast, lighter DM particles can induce a transition from a DM core to a halo structure, enhancing the maximum mass. Strong magnetic fields soften the equation of state and lower the DM content sustainable in the NS core before halo formation. Comparing our results with NICER and GW170817 observations, we constrain the range of viable DM parameters. Incorporating magnetic fields slightly shifts these limits, mainly affecting the maximum mass and tidal deformability. These findings provide new insights into the interplay between DM and magnetic fields in shaping the properties of neutron stars.
