Speaker
Description
This study examines the impact of dark matter (DM) on the bulk
properties of neutron stars (NS) using the relativistic mean field (RMF) theoretical
framework. The analysis considers the neutralino with a mass of 200 GeV, as the
DM candidate. This particle interacts with baryons via the standard Higgs boson.
The investigation focuses on how variations in the dark matter Fermi momentum
(k_f^DM) affect the neutron star equation of state (EOS) and key macroscopic
observables, including maximum mass (Mmax), canonical radius (R1.4), and
dimensionless tidal deformability (Λ1.4). The NLD, IOPB, and G3 parameter sets
are employed for this analysis. The presence of DM consistently softens the EOS,
resulting in systematic decreases in Mmax, R1.4, and Λ1.4. For example, within
the NLD parameter set, Mmax decreases from 2.353 solar masses to 1.955 solar
masses, and R1.4 decreases by approximately 3.8 km as k_f^DM increases from 0
to 0.05 GeV. A third order polynomial relationships of the form R1.4, Λ1.4
=a(k_f^DM )^3+b(k_f^DM )^2+c(k_f^DM )+d are established for all parameter sets.
The functional form of this correlation is same for all parameter set while
correlation coefficients a, b, c, and d depend on the specific parameter set and the
baryonic composition. When k_f^DM is in the range of 0.04 to 0.05 GeV, certain
RMF parameter sets that were previously inconsistent with gravitational-wave
constraints become compatible with observational limits from GW170817 and
Neutron Star Interior Composition Explorer (NICER) data.
