Spin-Down of the 65 Millisecond X-Ray Pulsar in the Supernova Remnant G11.2-0.3
著者
和文:
Torii, K.,
Tsunemi, H.,
Dotani, T.,
Mitsuda, K.,
河合 誠之,
Kinugasa, K.,
Saito, Y.,
Shibata, S..
英文:
Torii, K.,
Tsunemi, H.,
Dotani, T.,
Mitsuda, K.,
Kawai, N.,
Kinugasa, K.,
Saito, Y.,
Shibata, S..
言語
English
掲載誌/書名
和文:
英文:
Astrophysical Journal
巻, 号, ページ
Vol. 523
pp. L69-L72
出版年月
1999年9月
出版者
和文:
英文:
会議名称
和文:
英文:
開催地
和文:
英文:
アブストラクト
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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