Fig. 1

Gravitational mass versus central rest-mass density for NS models with different spins. The green shaded area is the region where no equilibrium models are possible because of excessive spin. The black solid lines are sequences of models that are non-rotating, Ω = 0, or rotating at break-up, Ω = ΩK, respectively (see text for more details). The arrows indicate example tracks of NSs with baryonic masses of 2.1, 2.3, and 2.4 M⊙ as they slow down due to magnetic braking.
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