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.
Testing dark decays of baryons in neutron stars
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
abstract
We demonstrate that the observation of neutron stars with masses greater than one solar mass places severe demands on any exotic neutron decay mode that could explain the discrepancy between beam and bottle measurements of the neutron lifetime. If the neutron can decay to a stable, feebly-interacting dark fermion, the maximum possible mass of a neutron star is 0.7 solar masses, while all well-measured neutron star masses exceed one solar mass. The survival of $2 M_\odot$ neutron stars therefore indicates that any explanation beyond the Standard Model for the neutron lifetime puzzle requires dark matter to be part of a multi-particle dark sector with highly constrained interactions.
citation-role summary
background 2
citation-polarity summary
roles
background 2polarities
background 2representative citing papers
A minimal dark matter model with one complex scalar carrying B and L numbers, stabilized by proton stability, with mass near the proton mass and relic density from UV freeze-in.
Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,
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%.
Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.
citing papers explorer
-
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.
-
Minimal Proton-Mass Dark Matter
A minimal dark matter model with one complex scalar carrying B and L numbers, stabilized by proton stability, with mass near the proton mass and relic density from UV freeze-in.
-
Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons
Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,
-
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%.
-
Bulk viscosity from neutron decays to dark baryons in neutron star matter
Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.