Current astronomical observations cannot definitively distinguish strange quark stars from neutron stars
2 events · 1 assessment
Assessed Supported
verdict confidence 0.85 · credence 0.92
Strange quark stars, hypothetical compact stars made of deconfined up, down, and strange quark matter, would closely resemble ordinary neutron stars in the properties astronomers can currently measure. The claim reflects the working position of the compact-star literature: because the two model families predict overlapping masses and radii over the observed range, mass and radius measurements from radio timing, X-ray pulse-profile modeling, and gravitational-wave tidal deformability constrain the equation of state without separating quark-matter from hadronic interpretations. Consistent with this, several observed compact stars remain viable strange-quark-star candidates, most prominently the unusually light central compact object in the supernova remnant HESS J1731-347, yet none has been confirmed as one, and even the two-solar-mass pulsar measurements are compatible with some quark-star equations of state. The main counter-consideration is that some phenomena already lean one way: pulsar glitches are difficult to explain with strange quark star models, which suggests at least the glitching pulsars are conventional neutron stars. But such arguments are model-dependent rather than decisive, and proposed clean discriminators, such as anomalously fast cooling, sub-millisecond rotation, post-merger gravitational-wave signatures, or a radius below what gravitationally bound matter allows, have not yet been observed at decisive precision. A confirmed detection of any such signature, or a definitive exclusion of quark-matter equations of state by future gravitational-wave and X-ray measurements, would overturn the claim.
Claim entered the graph