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Title: The binary nature of PSR J2032+4127

Abstract

PSR J2032+4127 is a γ-ray and radio-emitting pulsar which has been regarded as a young luminous isolated neutron star. However, its recent spin-down rate has extraordinarily increased by a factor of 2. Here we present evidence that this is due to its motion as a member of a highly-eccentric binary system with an ~15–M⊙ Be star, MT91 213. Timing observations show that, not only are the positions of the two stars coincident within 0.4 arcsec, but timing models of binary motion of the pulsar fit the data much better than a model of a young isolated pulsar. MT91 213, and hence the pulsar, lie in the Cyg OB2 stellar association, which is at a distance of only 1.4–1.7 kpc. The pulsar is currently on the near side of, and accelerating towards, the Be star, with an orbital period of 20–30 yr. Finally, the next periastron is well constrained to occur in early 2018, providing an opportunity to observe enhanced high-energy emission as seen in other Be-star binary systems.

Authors:
 [1];  [1];  [1];  [2];  [3];  [4];  [5]
  1. Univ. of Manchester (United Kingdom). School of Physics and Astronomy, Jodrell Bank Centre for Astrophysics
  2. Naval Research Lab. (NRL), Washington, DC (United States). Space Science Division
  3. CSIRO Astronomy and Space Science, Epping, NSW (Australia). Australia Telescope National Facility
  4. Columbia Univ., New York, NY (United States). Columbia Astrophysics Lab.
  5. George Mason Univ., Fairfax, VA (United States). College of Science
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF)
OSTI Identifier:
1354933
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 451; Journal Issue: 1; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; binaries; eclipsing; stars; Cyg OB2; starts neutron; MT91 213; Be stars

Citation Formats

Lyne, A. G., Stappers, B. W., Keith, M. J., Ray, P. S., Kerr, M., Camilo, F., and Johnson, T. J. The binary nature of PSR J2032+4127. United States: N. p., 2015. Web. doi:10.1093/mnras/stv236.
Lyne, A. G., Stappers, B. W., Keith, M. J., Ray, P. S., Kerr, M., Camilo, F., & Johnson, T. J. The binary nature of PSR J2032+4127. United States. https://doi.org/10.1093/mnras/stv236
Lyne, A. G., Stappers, B. W., Keith, M. J., Ray, P. S., Kerr, M., Camilo, F., and Johnson, T. J. 2015. "The binary nature of PSR J2032+4127". United States. https://doi.org/10.1093/mnras/stv236. https://www.osti.gov/servlets/purl/1354933.
@article{osti_1354933,
title = {The binary nature of PSR J2032+4127},
author = {Lyne, A. G. and Stappers, B. W. and Keith, M. J. and Ray, P. S. and Kerr, M. and Camilo, F. and Johnson, T. J.},
abstractNote = {PSR J2032+4127 is a γ-ray and radio-emitting pulsar which has been regarded as a young luminous isolated neutron star. However, its recent spin-down rate has extraordinarily increased by a factor of 2. Here we present evidence that this is due to its motion as a member of a highly-eccentric binary system with an ~15–M⊙ Be star, MT91 213. Timing observations show that, not only are the positions of the two stars coincident within 0.4 arcsec, but timing models of binary motion of the pulsar fit the data much better than a model of a young isolated pulsar. MT91 213, and hence the pulsar, lie in the Cyg OB2 stellar association, which is at a distance of only 1.4–1.7 kpc. The pulsar is currently on the near side of, and accelerating towards, the Be star, with an orbital period of 20–30 yr. Finally, the next periastron is well constrained to occur in early 2018, providing an opportunity to observe enhanced high-energy emission as seen in other Be-star binary systems.},
doi = {10.1093/mnras/stv236},
url = {https://www.osti.gov/biblio/1354933}, journal = {Monthly Notices of the Royal Astronomical Society},
issn = {0035-8711},
number = 1,
volume = 451,
place = {United States},
year = {Fri May 22 00:00:00 EDT 2015},
month = {Fri May 22 00:00:00 EDT 2015}
}

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Works referencing / citing this record:

Modelling the interaction between relativistic and non-relativistic winds in binary pulsar systems: strong magnetization of the pulsar wind
journal, October 2019


The prospects of pulsar timing with new-generation radio telescopes and the Square Kilometre Array
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Recurrent Outbursts Revealed in 3XMM J031820.8-663034
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Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron
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The Likely Fermi Detection of the Be X-Ray Binary GRO J1008-57
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A Very High Energy γ -Ray Survey toward the Cygnus Region of the Galaxy
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Phenomenology of gamma-ray emitting binaries
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Optical Spectral Evolution of the Gamma-Ray Binary PSR J2032+4127/MT91 213 Toward Its 2017 Periastron Passage
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The X-Ray Modulation of PSR J2032+4127/MT91 213 during the Periastron Passage in 2017
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