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1998). Thermal properties and detectability of neutron stars. II. Thermal evolution of rotation-powered neutron stars. Phys Rep, 292:1–130. van den Bergh, S. (1978). Observations of the Optical Remnant of SN 1181 = 3C 58. ApJL, 220:L9. , Downes, T. , and Keegan, R. (2004). An evolutionary model for pulsardriven supernova remnants. A hydrodynamical model. A&A, 420:937–944. Weisskopf, M. , Hester, J. , Tennant, A. , Elsner, R. , Schulz, N. , Marshall, H. , Nichols, J. , Swartz, D. , Kolodziejczak, J.

2002). New constraints on neutron star cooling from Chandra observations of 3C 58. ApJ, 571:L45–L49. Tsuruta, S. (1998). Thermal properties and detectability of neutron stars. II. Thermal evolution of rotation-powered neutron stars. Phys Rep, 292:1–130. van den Bergh, S. (1978). Observations of the Optical Remnant of SN 1181 = 3C 58. ApJL, 220:L9. , Downes, T. , and Keegan, R. (2004). An evolutionary model for pulsardriven supernova remnants. A hydrodynamical model. A&A, 420:937–944. Weisskopf, M.

1 from such d → h → e strongly suggest that the exceptionally fast MSPs they evolve into should usually have a surface magnetic field resembling that from an orthogonal dipole positioned on the NS spin-axis at the interface between the NS’s perfectly diamagnetic p-sc core and the bottom of its crust (Fig. 3b). A second large MSP family there should consist of almost aligned rotators (less frequently observed since their radio beams are directed so close to the NS spin-axes) whose µ⊥ have been “spin-up squeezed" to negligible strength.

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