High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213
High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213
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DOI：
10.3847/1538-4357/aa5c80
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发表时间：
2017-02
期刊：
影响因子：
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通讯作者：
J. Takata;P. Tam;C. Ng;K. L. Li;A. Kong;C. Hui;K. Cheng
中科院分区：
文献类型：
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作者：
J. Takata;P. Tam;C. Ng;K. L. Li;A. Kong;C. Hui;K. Cheng
PSR J2032+4127是一颗发出无线电波的伽马射线脉冲星，它围绕着一颗高质量的Be型星星运行，轨道周期长达25-50年，并且正在接近近星点，这将发生在2017年底/2018年初。该系统由一颗年轻的脉冲星和一颗Be型星星组成，它类似于所谓的伽马射线双星PSR B1259-63/LS 2883。因此，预计PSR J2032+4127显示出由脉冲星风和Be风/近星盘之间的相互作用引起的高能发射增强。Ho等人最近报道了来自该系统的X射线通量的快速增加。在本文中，我们还证实了快速增加的X射线通量沿着轨道，而GeV通量没有显着的变化。我们讨论了脉冲星风和星风相互作用引起的激波的高能辐射，并研究了脉冲星风在这一双星系统中的性质。我们认为Swift观测到的X射线通量的增加率表明（1）两风相互作用区域的动量比沿着轨道的变化，或者（2）脉冲星风的磁化参数随离脉冲星径向距离的演化。我们还讨论了脉冲星风/Be盘在近星通道的相互作用，并提出了在脉冲星周围形成吸积盘的可能性。我们通过冷相对论脉冲星风从吸积盘软光子的逆康普顿散射过程模拟高能量的排放。
PSR J2032+4127 is a radio-loud gamma-ray-emitting pulsar; it is orbiting around a high-mass Be type star with a very long orbital period of 25–50 years, and is approaching periastron, which will occur in late 2017/early 2018. This system comprises a young pulsar and a Be type star, which is similar to the so-called gamma-ray binary PSR B1259–63/LS2883. It is expected therefore that PSR J2032+4127 shows an enhancement of high-energy emission caused by the interaction between the pulsar wind and Be wind/disk around periastron. Ho et al. recently reported a rapid increase in the X-ray flux from this system. In this paper, we also confirm a rapid increase in the X-ray flux along the orbit, while the GeV flux shows no significant change. We discuss the high-energy emissions from the shock caused by the pulsar wind and stellar wind interaction and examine the properties of the pulsar wind in this binary system. We argue that the rate of increase of the X-ray flux observed by Swift indicates (1) a variation of the momentum ratio of the two-wind interaction region along the orbit, or (2) an evolution of the magnetization parameter of the pulsar wind with the radial distance from the pulsar. We also discuss the pulsar wind/Be disk interaction at the periastron passage, and propose the possibility of formation of an accretion disk around the pulsar. We model high-energy emissions through the inverse-Compton scattering process of the cold-relativistic pulsar wind off soft photons from the accretion disk.