High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213

J. Takata, P. H.T. Tam, C. W. Ng, K. L. Li, A. K.H. Kong, C. Y. Hui, K. S. Cheng

研究成果: Article同行評審

27 引文 斯高帕斯(Scopus)

摘要

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.

原文English
文章編號241
期刊Astrophysical Journal
836
發行號2
DOIs
出版狀態Published - 2017 二月 20

All Science Journal Classification (ASJC) codes

  • 天文和天體物理學
  • 空間與行星科學

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