Kavli Affiliate: Renxin Xu
| First 5 Authors: Chen Zhang, Chen Zhang, , ,
| Summary:
Some recent pulsar observations cannot naturally fit into the conventional
picture of neutron stars: the compact objects associated with HESS J1731-347
and XTE J1814-338 have too small radii at the low-mass regime, while the
secondary component of GW190814 is too massive for neutron stars to be
compatible with constraints from the GW170817 event. In this study, we
demonstrate that all these anomalous observations and tensions, together with
other conventional ones such as recent NICER observations of PSR J0740+6620,
J0030+0451, and PSR J0437-4715, can be naturally explained simultaneously by a
new general type of hybrid stars that are self-bound and radially stable in the
slow phase transition context, and by some subsets even in the rapid phase
transition context also. As a proof of concept, we use hybrid quark stars,
inverted hybrid stars, and hybrid strangeon stars as benchmark examples to
explicitly demonstrate the advantage and feasibility of slow stable self-bound
hybrid stars in relieving all tensions related to compact stars’ masses, radii,
and tidal deformabilities.
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