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Title:
Spin-Down of the 65 Millisecond X-Ray Pulsar in the Supernova Remnant G11.2-0.3
Authors:
Torii, Ken'ichi; Tsunemi, Hiroshi; Dotani, Tadayasu; Mitsuda, Kazuhisa; Kawai, Nobuyuki; Kinugasa, Kenzo; Saito, Yoshitaka; Shibata, Shinpei
Publication:
The Astrophysical Journal, Volume 523, Issue 1, pp. L69-L72. (ApJL Homepage)
Publication Date:
09/1999
Origin:
APJ
ApJ Keywords:
STARS: PULSARS: GENERAL, STARS: PULSARS: INDIVIDUAL: ALPHANUMERIC: AX J1811.5-1926, STARS: SUPERNOVAE: INDIVIDUAL: ALPHANUMERIC: G11.2-0.3, X-RAYS: GENERAL
DOI:
10.1086/312251
Bibliographic Code:
1999ApJ...523L..69T

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 P=(4.40^+0.03_-0.04)x10^-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=1.7x10^12 G) and the characteristic age [P/(2P)=2.4x10^4 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 P. If the pulsar was formed during the historical event, the initial pulse period should have been relatively slow (P_0~=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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