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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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.
Brown dwarfs modeled with a self-interacting dark matter fluid component show modified radii and second-order Love numbers due to core accumulation.
citing papers explorer
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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.
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Self-Interacting Dark Matter in Brown Dwarfs
Brown dwarfs modeled with a self-interacting dark matter fluid component show modified radii and second-order Love numbers due to core accumulation.