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.
Cooling of dark neutron stars,
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
verdicts
UNVERDICTED 3representative citing papers
Dark matter cores heat baryonic matter in evolving proto-neutron stars by deepening the gravitational potential while halos cool it, providing a diagnostic distinct from hyperons.
DM admixture in isentropic neutron stars can mimic quark-matter conformality signatures via competition between thermal effects and dark sector softening.
citing papers explorer
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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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Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach
Dark matter cores heat baryonic matter in evolving proto-neutron stars by deepening the gravitational potential while halos cool it, providing a diagnostic distinct from hyperons.
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Observables and conformal properties of dark matter admixed isentropic neutron stars
DM admixture in isentropic neutron stars can mimic quark-matter conformality signatures via competition between thermal effects and dark sector softening.