Speaker
Description
In this work, we present the first investigation of dark matter-admixed
quarkyonic stars (DAQSs) using a two-fluid framework. The visible sector of the
star is described through a quarkyonic equation of state (EOS) based on the
Effective Relativistic Mean Field (E-RMF) model, while the DM component is
modeled as a degenerate fermionic gas with scalar and vector self-interaction
terms. Our study begins with the mass-radius characteristics, demonstrating that
the addition of DM allows stellar configurations to attain masses consistent with the
GW190814 event. Depending on the EOS, we uncover two possible morphologies:
DM-core dominated and DM-halo dominated stars, each associated with distinct
structural features. By fixing the stellar mass within the GW190814 range, we
constrain the viable DM fractions and assess the impact of different interaction
channels. With the resulting EOSs, we extend our analysis to tidal deformability
and stellar radii, observing compatibility with the constraints from GW170817,
GW190814, and NICER. We then summarize the key properties of DAQSs
covering EOS type, DM content, morphology, and observable quantities-in a
comparative overview. Altogether, this work establishes a coherent two-fluid
description for probing dense QCD matter and DM in the multi-messenger context,
and supports the interpretation of the GW190814 secondary as either a DM-core
or DM-halo quarkyonic star.
