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.
Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
3 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We obtain a new equation of state for the nucleonic and hyperonic inner core of neutron stars that fulfills the 2$M_{\odot}$ observations as well as the recent determinations of stellar radii below 13 km. The nucleonic equation of state is obtained from a new parametrization of the FSU2 relativistic mean-field functional that satisfies these latest astrophysical constraints and, at the same time, reproduces the properties of nuclear matter and finite nuclei while fulfilling the restrictions on high-density matter deduced from heavy-ion collisions. On the one hand, the equation of state of neutron star matter is softened around saturation density, which increases the compactness of canonical neutron stars leading to stellar radii below 13 km. On the other hand, the equation of state is stiff enough at higher densities to fulfill the 2$M_{\odot}$ limit. By a slight modification of the parametrization, we also find that the constraints of 2$M_{\odot}$ neutron stars with radii around 13 km are satisfied when hyperons are considered. The inclusion of the high magnetic fields present in magnetars further stiffens the equation of state. Hyperonic magnetars with magnetic fields in the surface of $ \sim 10^{15}$ G and with values of $\sim 10^{18}$ G in the interior can reach maximum masses of 2$M_{\odot}$ with radii in the 12-13 km range.
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Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.
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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Neutron star with dark matter using vector portal
Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.
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Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.