毫秒脉冲星
物理
脉冲星
天体物理学
中子星
毫秒
X射线脉冲星
天文
双星脉冲星
增值(金融)
双星
二进制数
低质量
X射线二进制
脉冲星行星
星星
算术
数学
作者
Anne M. Archibald,I. H. Stairs,S. M. Ransom,V. M. Kaspi,V. I. Kondratiev,D. R. Lorimer,M. A. McLaughlin,J. Boyles,J. W. T. Hessels,Ryan S. Lynch,J. van Leeuwen,M. S. Roberts,F. A. Jenet,D. J. Champion,Rachel A. Rosen,B. N. Barlow,B. H. Dunlap,Ronald A. Remillard
出处
期刊:Science
[American Association for the Advancement of Science (AAAS)]
日期:2009-06-12
卷期号:324 (5933): 1411-1414
被引量:489
标识
DOI:10.1126/science.1172740
摘要
From X-ray Binary to Pulsar Pulsars with millisecond rotational periods are thought to originate from neutron stars in low-mass x-ray binaries that had their spin frequencies increased by long-lasting mass transfer from their companion stars. Using data from a radio pulsar survey, Archibald et al. (p. 1411 , published online 21 May; see the Perspective by Kramer ) found a neutron star in a low-mass X-ray binary that is in the process of turning into a radio millisecond pulsar. The system, which consists of a solar-like star and a 1.69-millisecond radio pulsar, has gone through a recent accretion phase, characteristic of low-mass X-ray binaries, but it shows no accretion disk anymore, confirming the evolutionary connection between millisecond radio pulsars and low-mass X-ray binaries.
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