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Dark matter admixed neutron stars
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Dark matter admixed neutron stars
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Neutron stars could contain a mixture of ordinary nuclear matter and dark matter, such that dark matter could influence observable properties of the star, such as its mass and radius. We study these dark matter admixed neutron stars for two choices of dark matter: a free Fermi gas and mirror dark matter. In addition to solving the multi-fluid Tolman-Oppenheimer-Volkoff equations for static solutions and presenting mass-radius diagrams, we focus on two computations that are lacking in the literature. The first is a rigorous determination of stability over the whole of parameter space, which we do using two different methods. The first method is based on harmonic time-dependent perturbations to the static solutions and on solving for the radial oscillation frequency. The second method, which is less well-known, conveniently makes use of unperturbed, static solutions only. The second computation is of the radial oscillation frequency, for fundamental modes, over large swaths of parameter space.
Forward citations
Cited by 11 Pith papers
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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-energ...
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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...
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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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Rotating Fermion-Boson Stars in $R$-squared Gravity
R-squared gravity enlarges the equilibrium domain of rotating fermion-boson stars and raises static and Keplerian maximum masses relative to GR while remaining compatible with current compact-object 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-st...
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A self-consistent Higgs-portal framework for dark matter--admixed neutron stars: Collider-motivated benchmarks meet multimessenger constraints
Adding heavy dark matter to neutron stars via nχ=FχnB softens the equation of state and lowers the maximum mass, but the vector interaction invoked is numerically negligible.
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The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations
Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-per...
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Stability Boundary of Neutron-Dark Matter Mixed Stars
For two-fluid neutron–dark-matter stars, the paper claims a rigorous equivalence between the static critical-curve stability criterion and the vanishing of a radial oscillation mode, and maps the resulting stable conf...
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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.
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Effects of dark matter and magnetic field on neutron star properties in relativistic mean-field theory: A single-fluid approach
Fermionic dark matter and strong central magnetic fields both reduce neutron-star maximum mass and radius and lower tidal deformability in single-fluid RMF models, remaining compatible with GW/NICER constraints over t...
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