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.
Neutron Stars as Dark Matter Probes
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abstract
We examine whether the accretion of dark matter onto neutron stars could ever have any visible external effects. Captured dark matter which subsequently annihilates will heat the neutron stars, although it seems the effect will be too small to heat close neutron stars at an observable rate whilst those at the galactic centre are obscured by dust. Non-annihilating dark matter would accumulate at the centre of the neutron star. In a very dense region of dark matter such as that which may be found at the centre of the galaxy, a neutron star might accrete enough to cause it to collapse within a period of time less than the age of the Universe. We calculate what value of the stable dark matter-nucleon cross section would cause this to occur for a large range of masses.
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Bose-Einstein condensate formation in neutron stars enhances dark matter annihilation by 10^15-10^20, allowing freeze-in models to produce observable heating and probe neutrino-fog scattering cross-sections.
Muonphilic portals to fermionic asymmetric dark matter are constrained by existing data and can be probed further by 3 and 10 TeV muon colliders.
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.
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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Probing freeze-in dark matter using Bose-Einstein condensate in neutron star
Bose-Einstein condensate formation in neutron stars enhances dark matter annihilation by 10^15-10^20, allowing freeze-in models to produce observable heating and probe neutrino-fog scattering cross-sections.
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Muonphilic asymmetric dark matter at a future muon collider
Muonphilic portals to fermionic asymmetric dark matter are constrained by existing data and can be probed further by 3 and 10 TeV muon colliders.
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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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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.