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

Abstract

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.more » 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.« less

Authors:
 [1];  [2]; ;  [3];  [4];  [5];  [6]
  1. School of physics, Huazhong University of Science and Technology, Wuhan 430074 (China)
  2. Institute of Astronomy and Space Science, Sun Yat-Sen University, Guangzhou 510275 (China)
  3. Department of Physics, The University of Hong Kong, Pokfulam Road (Hong Kong)
  4. Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824-2320 (United States)
  5. Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan (China)
  6. Department of Astronomy and Space Science, Chungnam National University, Daejeon 305-764 (Korea, Republic of)
Publication Date:
OSTI Identifier:
22663754
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 836; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; COMPTON EFFECT; EMISSION; EVOLUTION; GAMMA RADIATION; GEV RANGE; MAGNETIZATION; MASS; PHOTONS; PULSARS; RELATIVISTIC RANGE; STARS; STELLAR WINDS; X RADIATION

Citation Formats

Takata, J., Tam, P. H. T., Ng, C. W., Cheng, K. S., Li, K. L., Kong, A. K. H., and Hui, C. Y., E-mail: takata@hust.edu.cn. High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA5C80.
Takata, J., Tam, P. H. T., Ng, C. W., Cheng, K. S., Li, K. L., Kong, A. K. H., & Hui, C. Y., E-mail: takata@hust.edu.cn. High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213. United States. doi:10.3847/1538-4357/AA5C80.
Takata, J., Tam, P. H. T., Ng, C. W., Cheng, K. S., Li, K. L., Kong, A. K. H., and Hui, C. Y., E-mail: takata@hust.edu.cn. Mon . "High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213". United States. doi:10.3847/1538-4357/AA5C80.
@article{osti_22663754,
title = {High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213},
author = {Takata, J. and Tam, P. H. T. and Ng, C. W. and Cheng, K. S. and Li, K. L. and Kong, A. K. H. and Hui, C. Y., E-mail: takata@hust.edu.cn},
abstractNote = {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.},
doi = {10.3847/1538-4357/AA5C80},
journal = {Astrophysical Journal},
number = 2,
volume = 836,
place = {United States},
year = {Mon Feb 20 00:00:00 EST 2017},
month = {Mon Feb 20 00:00:00 EST 2017}
}