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PreprintCC BY-NC-SA 4.0arXiv

Relativistic effects of PSR~J1856--0039 double neutron star system in a 2.36-hour compact orbit

  • Z. L. Yang
  • J. L. Han
  • W. Q. Su
  • P. F. Wang
  • C. Wang
  • T. Wang
  • D. J. Zhou
  • Yi Yan
  • J. Xu
  • W. C. Jing
  • N. N. Cai
  • R. X. Xu
2 more authors
  • H. G. Wang
  • X. P. You
Open at sourcePDFDOICite

Abstract

Compact double neutron star (DNS) systems are unique laboratories for testing gravitational theories and studying DNS mergers. Here we report the properties of a new DNS system, PSR J1856--0039, discovered in the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The pulsar is mildly recycled with a period of 23.4~ms in a compact eccentric orbit (e=0.106) with an orbital period of 2.36 hours. By following up FAST observations, we measured the relativistic effects, including the orbital period derivative Ṗorb=−1.284±0.019×10−12 s s−1, periastron advance ω̇=17.5859±0.0007 deg yr−1, and Einstein delay γ=0.445±0.011 ms. This DNS system has a low orbital inclination of i=133∘.2±1∘.1 and the lowest total mass of any known DNS, Mtot=2.48841±0.00015 M⊙, with a determined pulsar mass of 1.304±0.022 M⊙ and a companion mass of 1.185±0.022 M⊙, one of the lowest neutron-star masses. The observed orbital decay due to gravitational-wave emission ṖGWorb,obs and the orbital decay predicted by general relativity ṖGWorb,pred are consistent at a level of ṖGWorb,obs/ṖGWorb,pred=1.009(14) (68% confidence). This DNS will merge after 82 Myr and may form a stable neutron star or collapse into a black hole after spin-down. Long-term monitoring could potentially probe the Lense-Thirring precession.

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Cite

BibTeXRIS
BibTeX
@misc{yang2026relativistic,
  title = {{Relativistic effects of PSR~J1856--0039 double neutron star system in a 2.36-hour compact orbit}},
  author = {Z. L. Yang and J. L. Han and W. Q. Su and P. F. Wang and C. Wang and T. Wang and D. J. Zhou and Yi Yan and J. Xu and W. C. Jing and N. N. Cai and R. X. Xu and H. G. Wang and X. P. You},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2607.27333},
  eprint = {2607.27333},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2607.27333},
  note = {CC BY-NC-SA 4.0},
}
RIS
TY  - UNPB
TI  - Relativistic effects of PSR~J1856--0039 double neutron star system in a 2.36-hour compact orbit
AU  - Z. L. Yang
AU  - J. L. Han
AU  - W. Q. Su
AU  - P. F. Wang
AU  - C. Wang
AU  - T. Wang
AU  - D. J. Zhou
AU  - Yi Yan
AU  - J. Xu
AU  - W. C. Jing
AU  - N. N. Cai
AU  - R. X. Xu
AU  - H. G. Wang
AU  - X. P. You
PY  - 2026
DA  - 2026/09/16
PB  - arXiv
DO  - 10.48550/arxiv.2607.27333
UR  - https://arxiv.org/abs/2607.27333
AB  - Compact double neutron star (DNS) systems are unique laboratories for testing gravitational theories and studying DNS mergers. Here we report the properties of a new DNS system, PSR J1856--0039, discovered in the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The pulsar is mildly recycled with a period of 23.4~ms in a compact eccentric orbit (e=0.106) with an orbital period of 2.36 hours. By following up FAST observations, we measured the relativistic effects, including the orbital period derivative Ṗ_orb=−1.284±0.019×10^−12 s s^−1, periastron advance ω̇=17.5859±0.0007 deg yr^−1, and Einstein delay γ=0.445±0.011 ms. This DNS system has a low orbital inclination of i=133^∘.2±1^∘.1 and the lowest total mass of any known DNS, M_tot=2.48841±0.00015 M⊙, with a determined pulsar mass of 1.304±0.022 M_⊙ and a companion mass of 1.185±0.022 M_⊙, one of the lowest neutron-star masses. The observed orbital decay due to gravitational-wave emission Ṗ^GW_orb,obs and the orbital decay predicted by general relativity Ṗ^GW_orb,pred are consistent at a level of Ṗ^GW_orb,obs/Ṗ^GW_orb,pred=1.009(14) (68% confidence). This DNS will merge after 82 Myr and may form a stable neutron star or collapse into a black hole after spin-down. Long-term monitoring could potentially probe the Lense-Thirring precession.
ER  -