大地岁差对用条纹风模型导出的脉冲星高能脉冲轮廓演化的影响
Effect of geodetic precession on the evolution of pulsar high-energy pulse profiles as derived with the striped-wind model
摘要：
在双脉冲星系统PSR J 0737 -3039中直接观测到大地岁差。它的速率甚至被测量过，并且与广义相对论的预测一致。最近，在X射线和伽马射线中发现了双脉冲星。这激发了在该系统的高能脉冲轮廓中观察大地岁差的希望。不幸的是，二进制的几何配置使任何检测到这种影响不太可能。然而，这种进动可能存在于其他至少包含一颗X射线或伽马射线脉冲星的相对论双星或双中子星系统中。{We根据条纹风模型，计算预期来自这种大地运动的高能脉冲轮廓的变化。我们比较我们的结果与两极焦散和外间隙发射模式。{For如果轨道角动量和自旋角动量之间存在足够的不对准，则预期在X射线和伽马射线能带中，由于测地岁差而导致的脉冲轮廓的显著变化。{The条纹风的基本特征在几个曲线图中示出，这些曲线图示出了脉冲强度的最大值的演变、两个峰的分离（如果存在的话）以及每个峰的宽度的变化。我们强调了与其他竞争高能模型的主要区别。{We对未来可能探测到的具有最高自旋进动率的双中子星系统的高能辐射做出一些预测。这样的观测肯定会有利于一些脉冲高能发射的情况。
英文摘要：
Geodetic precession has been observed directly in the double-pulsar system PSR J0737-3039. Its rate has even been measured and agrees with predictions of general relativity. Very recently, the double pulsar has been detected in X-rays and gamma-rays. This fuels the hope observing geodetic precession in the high-energy pulse profile of this system. Unfortunately, the geometric configuration of the binary renders any detection of such an effect unlikely. Nevertheless, this precession is probably present in other relativistic binaries or double neutron star systems containing at least one X-ray or gamma-ray pulsar.}{We compute the variation of the high-energy pulse profile expected from this geodetic motion according to the striped-wind model. We compare our results with two-pole caustic and outer gap emission patterns.}{For a sufficient misalignment between the orbital angular momentum and the spin angular momentum, a significant change in the pulse profile as a result of geodetic precession is expected in the X-ray and gamma-ray energy band.}{The essential features of the striped wind are indicated in several plots showing the evolution of the maximum of the pulsed intensity, the separation of both peaks, if present, and the variation in the width of each peak. We highlight the main differences with other competing high-energy models.}{We make some predictions about possible future detection of high-energy emission from double neutron star systems with the highest spin precession rate. Such observations will definitely favour some pulsed high-energy emission scenarios.
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