Models of dense matter can be tested by comparing neutron star radii R determined from observations with theoretical predictions. Let us remind that R denotes the circumferential stellar radius (§ 6.1). Unfortunately, for typical neutron star masses between 1 and 2 Mq, the radius is not very sensitive to the EOS (§ 6.6.1). As can be deduced from Fig.6.5, in order to really distinguish between the different EOSs, one has to measure the radius with a precision of ~ 0.5 km (within statistical significance of 2a or better).
Let us outline several methods to evaluate the neutron star radius from observations. First of all, one can infer the radius by measuring zsurf and the stellar mass M:
(1 + -W)2 2GM M , r = ¿f(S + W)"■ " = — & 2-95 mq (9-27)
Was this article helpful?