Extended Data Fig. 4: Magneto-thermal evolutionary models for neutron stars assuming different initial magnetic-field strengths and configurations.
From: Detection of X-ray emission from a bright long-period radio transient
(a) Evolution in the \(P-\mathop{P}\limits^{.}\) plane. Dashed (solid) lines correspond to theoretical death lines for a pure dipole (highly multipolar) configuration18,19. The grey-shaded region indicates the radio pulsar ‘death valley’ between the two extreme configurations. (b) Evolution of the quiescent X-ray luminosity as a function of the rotational power (\(\mathop{E}\limits^{.}\)). The grey line is \({L}_{X}=\mathop{E}\limits^{.}\) while the grey shaded area represents the constraints for ASKAP J1832–0911 during quiescence. See10,77,78 and references therein for details on the theoretical cooling models and the plotted sources.
