Determination of the Geometry of the PSR B1913+16 System by Geodetic Precession
Determination of the Geometry of the PSR B1913+16 System by Geodetic Precession
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DOI：
10.1086/306535
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发表时间：
1998-08
期刊：
影响因子：
--
通讯作者：
M. Kramer
中科院分区：
文献类型：
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作者：
M. Kramer
本文介绍了脉冲双星B1913+16的新观测结果。自1978年以来，脉冲轮廓的主导分量已急剧减弱约40%。第一次，减少组件分离观察，符合预期的大地岁差。假设广义相对论和圆形空心锥状光束的正确性，一个完全一致的模型系统的几何形状的发展。脉冲星自旋和轨道动量之间的错位角的确定，直接证据的不对称踢在第二次超新星爆炸。据认为，轨道倾角是132.°8（而不是47.°2）。该模型预测PSR B1913+16在2025年后将不再可观测。
New observations of the binary pulsar B1913+16 are presented. Since 1978 the leading component of the pulse profile has weakened dramatically by about 40%. For the first time, a decrease in component separation is observed, consistent with expectations of geodetic precession. Assuming the correctness of general relativity and a circular hollow-cone-like beam, a fully consistent model for the system geometry is developed. The misalignment angle between pulsar spin and orbital momentum is determined, giving direct evidence for an asymmetric kick during the second supernova explosion. It is argued that the orbital inclination angle is 132.°8 (rather than 47.°2). A prediction of this model is that PSR B1913+16 will no longer be observable after the year 2025.