Spin-Down of the 65 Millisecond X-Ray Pulsar in the Supernova Remnant G11.2−0.3

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Abstract
We report here the first measurement of the spin-down rate of the 65 ms X-ray pulsar within the supernova remnant G11.2-0.3. The period derivative is measured to be = (4.40) × 10-14 s s-1 using the Advanced Satellite for Cosmology and Astrophysics and BeppoSAX. From the pulsar period and its derivative, the corresponding surface magnetic field (B = 1.7 × 1012 G) and the characteristic age [P/(2) = 2.4 × 104 yr] are derived. The physical association of the pulsar and supernova remnant with the historical record of A.D. 386 is discussed in the context of the measured . If the pulsar was formed during the historical event, the initial pulse period should have been relatively slow (P0 62 ms). This initial period is more than a factor of 3 larger than that of a small number of prototypical objects, suggesting a diversity of initial periods for newly formed neutron stars.

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