neutronstarlike

Neutronstarlike is a descriptive term used in astrophysics and related fields to refer to compact objects or observational states that closely resemble a neutron star in key properties, without asserting that the object is a canonical neutron star. In practice, it is used for theoretical models, candidate objects, or phases where the interior composition or external appearance approaches what is expected for neutron stars, but evidence remains incomplete.

Typical neutronstarlike objects are characterized by extreme densities, strong gravity, and, often, strong magnetic fields. Expected density near or above nuclear saturation, radii around 10 kilometers, and masses around 1 to a few solar masses. Magnetic fields may range from 10^12 to 10^15 gauss, and rotation can be rapid, with periods from milliseconds to a few seconds. Emission can be multimodal, including pulsed radio emission, thermal X-ray spectra from a hot surface, non-thermal X-ray and gamma-ray emission, and sometimes gravitational-wave signals if the object is deformed.

Neutronstarlike classifications can arise in several scenarios: as a post-supernova remnant containing a neutron-star-like core; as a quark star or hybrid star whose interior is composed of deconfined quarks or mixed phases; or as an observationally ambiguous compact object in which the exact interior composition is uncertain. The term is often used to compare theoretical models or observational data with canonical neutron stars, aiding investigations into the dense matter equation of state and the transition between different ultradense phases.

Observationally distinguishing neutronstarlike objects from true neutron stars or black holes relies on precise timing, spectroscopic measurements, and, where available, gravitational-wave data, to infer mass, radius, magnetic field, and rotational behavior.