A new relativistic linear perturbation formalism is derived for polar modes in gravitationally coupled two-fluid neutron stars, with numerical computation of representative f- and p-mode spectra classified by dominant fluid character.
Kain,Dark matter admixed neutron stars,Phys
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Strongly interacting dark matter described by a first-principles G2 gauge-theory equation of state can be mixed into neutron stars while remaining compatible with current observational constraints.
Increasing the bosonic dark matter fraction in admixed neutron stars shifts axial quasi-normal mode frequencies and damping times, can reorder mode hierarchy, and drives a transition from neutron-star-like to boson-star-like ringdown behavior.
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.
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
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Non-radial pulsations of gravitationally coupled two-fluid neutron stars in general relativity
A new relativistic linear perturbation formalism is derived for polar modes in gravitationally coupled two-fluid neutron stars, with numerical computation of representative f- and p-mode spectra classified by dominant fluid character.
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Strongly Interacting Dark Matter admixed Neutron Stars
Strongly interacting dark matter described by a first-principles G2 gauge-theory equation of state can be mixed into neutron stars while remaining compatible with current observational constraints.
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Axial Quasi-normal Modes of Admixed Neutron Stars
Increasing the bosonic dark matter fraction in admixed neutron stars shifts axial quasi-normal mode frequencies and damping times, can reorder mode hierarchy, and drives a transition from neutron-star-like to boson-star-like ringdown behavior.
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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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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.