Abstract
We investigated compact stars consisting of cold quark matter and fermionic dark matter treated as two admixed fluids. We computed the stellar structures and fundamental radial oscillation frequencies of different masses of the dark fermion in the cases of weak and strong self-interacting dark matter. We found that the fundamental frequency can be dramatically modified and, in some cases, stable dark strange planets and dark strangelets with very low masses and radii can be formed.
Highlights
Compact stars offer a variety of possibilities for probing the inner structure of matter through astronomical observations
We investigate strange quark stars consisting of cold quark matter (QM) and non selfannihilating fermionic cold dark matter (DM) treated as two admixed fluids, attracted only gravitationally
B = (145 MeV)4, i.e., ∼ 1 GeV/fm3. The reason for this is that higher values of are required when DM is present in the admixed star; (ii) the three values of DM c correspond to near the minimum, intermediate, and near the maximal-mass central densities for corresponding pure DM stars
Summary
Compact stars offer a variety of possibilities for probing the inner structure of matter through astronomical observations. Matter at extremely high densities can only be probed, so far, by investigating unique objects that represent one of the possible final stages of stellar evolution. The structure of compact stars can be determined by solving the Tolman–Oppenheimer–Volkov (TOV) equations, given the equation of state (EoS) for the matter under consideration [1,2]. For high enough central energy densities, one expects to find either hybrid stars, i.e., neutron stars with a quark matter (QM) core, or even more exotic objects, such as quark stars. For a review on quark matter in neutron stars, see Ref. For a review on quark matter in neutron stars, see Ref. [9]
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