Mirror dark matter admixture via mutual mean-field shifts softens the nuclear EOS, raises central densities, lowers maximum masses, and moves the direct Urca onset to higher or lower masses depending on symmetry-energy stiffness.
Thermalization and annihilation of dark matter in neutron stars,
7 Pith papers cite this work. Polarity classification is still indexing.
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Asymmetric cannibal dark matter with Z3-symmetric 3→2 interactions depletes in neutron star cores, producing observable heating signatures that constrain dark matter parameters beyond standard annihilation models.
A small vacuum-like dark-energy admixture in neutron stars with 400 MeV–1 GeV fermionic dark matter shrinks halo-induced radius differences from several kilometers to sub-kilometer scales and mass differences to ≲1%.
DM admixture in isentropic neutron stars can mimic quark-matter conformality signatures via competition between thermal effects and dark sector softening.
Observation of neutron stars at 1000-1200 K could constrain asymmetric dark matter self-interaction cross-sections by two orders of magnitude beyond bullet cluster limits.
Dipole dark matter produced by freeze-out or freeze-in, including entropy dilution from reheating, can be probed via neutron star heating due to momentum-dependent electromagnetic interactions.
DM-heated neutron stars in the Galactic Center reach equilibrium temperatures of 10^4-10^6 K but their emission is below detection thresholds due to extinction.
citing papers explorer
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A self-consistent single-fluid framework for neutron stars admixed with mirror dark matter
Mirror dark matter admixture via mutual mean-field shifts softens the nuclear EOS, raises central densities, lowers maximum masses, and moves the direct Urca onset to higher or lower masses depending on symmetry-energy stiffness.
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Asymmetric Cannibal Dark Matter: Constraints from Neutron Star
Asymmetric cannibal dark matter with Z3-symmetric 3→2 interactions depletes in neutron star cores, producing observable heating signatures that constrain dark matter parameters beyond standard annihilation models.
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Sub-GeV dark matter in neutron stars: halo morphologies and their suppression by vacuum-like pressure
A small vacuum-like dark-energy admixture in neutron stars with 400 MeV–1 GeV fermionic dark matter shrinks halo-induced radius differences from several kilometers to sub-kilometer scales and mass differences to ≲1%.
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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.
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Constraining dark matter self-interaction from kinetic heating in neutron stars
Observation of neutron stars at 1000-1200 K could constrain asymmetric dark matter self-interaction cross-sections by two orders of magnitude beyond bullet cluster limits.
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Neutron stars as thermometers for reheating induced dipole dark matter
Dipole dark matter produced by freeze-out or freeze-in, including entropy dilution from reheating, can be probed via neutron star heating due to momentum-dependent electromagnetic interactions.
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Thermal emission from dark matter-heated neutron stars in the Galactic Center
DM-heated neutron stars in the Galactic Center reach equilibrium temperatures of 10^4-10^6 K but their emission is below detection thresholds due to extinction.