Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.
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Vector-portal fermionic dark matter softens or stiffens the neutron-star equation of state depending on Z' mass, producing mass-radius and tidal-deformability signatures constrained by GW170817 and NICER.
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The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations
Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.
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Neutron star with dark matter using vector portal
Vector-portal fermionic dark matter softens or stiffens the neutron-star equation of state depending on Z' mass, producing mass-radius and tidal-deformability signatures constrained by GW170817 and NICER.