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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >An application of the Ghosh & Lamb model to the accretion-powered X-ray pulsar X Persei
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An application of the Ghosh & Lamb model to the accretion-powered X-ray pulsar X Persei

机译：Ghosh＆Lamb模型将Ghosh＆Lamb模型应用于Accretion-Powered X射线Pulsar X Persei

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摘要

The accretion-induced pulse period changes of the Be/X-ray binary pulsar X Persei were investigated over the period of 1996 January to 2017 September. This study utilized the monitoring data acquired with the RXTE All-Sky Monitor in 1.5-12 keV and the MAXI Gas-Slit Camera in 2-20 keV. The source intensity changed by a factor of 5-6 over this period. The pulsar was spinning down for 1996-2003, and has been spinning up since 2003, as already reported. The spin-up/down rate and the 3-12 keV flux, determined every 250 d, showed a clear negative correlation, which can be successfully explained by the accretion torque model proposed by Ghosh and Lamb (1979, ApJ, 234, 296). When the mass, radius, and distance of the neutron star were allowed to vary over a range of 1.0-2.4 solar masses, 9.5-15 km, and 0.77-0.85 kpc, respectively, the magnetic field strength of B = (4-25) x 10(13) G gave the best fits to the observations. In contrast, the observed results cannot be explained by the values of B similar to 10(12) G previously suggested for X Persei, as long as the mass, radius, and distance are required to take reasonable values. Assuming a distance of 0.81 +/- 0.04 kpc as indicated by optical astrometry, the mass of the neutron star is estimated as M = 2.03 +/- 0.17 solar masses.
机译：在1996年1月至2017年9月，调查了BE / X射线二元脉冲X Persei的增孔诱导的脉冲周期变化。本研究利用了在2-20keV中的1.5-12 kev和Maxi气隙相机中使用RXTE全天监测器获取的监测数据。在此期间，源强度会在5-6倍的5-6倍。脉冲柱在1996 - 2003年旋转下来，自2003年以来一直在旋转，如图所示。每250d确定旋转/下降率和3-12keV通量显示出明显的负相关性，可以通过Ghosh和Lamb（1979，APJ，234,296）提出的增速扭矩模型成功解释。当中子星的质量，半径和距离分别在1.0-2.4太阳质量范围内变化，分别为1.0-2.4，9.5-15 km和0.77-0.85 kpc，磁场强度B =（4-25 ）x 10（13）g给出了观察结果的最佳拟合。相反，观察结果不能通过前面建议的类似于10（12）G的B值，只要质量，半径和距离需要合理的值。假设如光学天空测量级所示的距离为0.81 +/- 0.04kpc，所以中子星的质量估计为M = 2.03 +/- 0.17太阳能质量。

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