The High Time Resolution Universe Pulsar Survey - XIII. PSR J1757-1854, the most accelerated binary pulsar

Research output: Contribution to journalArticle

  • External authors:
  • A. D. Cameron
  • D. J. Champion
  • M. Kramer
  • M. Bailes
  • E. D. Barr
  • C. G. Bassa
  • S. Bhandari
  • N. D. R. Bhat
  • M. Burgay
  • S. Burke-Spolaor
  • R. P. Eatough
  • C. M. L. Flynn
  • P. C. C. Freire
  • A. Jameson
  • S. Johnston
  • R. Karuppusamy
  • L. Levin
  • D. R. Lorimer
  • A. G. Lyne
  • M. A. McLaughlin
  • C. Ng
  • E. Petroff
  • A. Possenti
  • A. Ridolfi
  • B. W. Stappers
  • W. van Straten
  • T. M. Tauris
  • C. Tiburzi
  • N. Wex

Abstract

We report the discovery of PSR J1757$-$1854, a 21.5-ms pulsar in a highly-eccentric, 4.4-h orbit around a neutron star (NS) companion. PSR J1757$-$1854 exhibits some of the most extreme relativistic parameters of any known pulsar, including the strongest relativistic effects due to gravitational-wave (GW) damping, with a merger time of 76 Myr. Following a 1.6-yr timing campaign, we have measured five post-Keplerian (PK) parameters, yielding the two component masses ($m_\text{p}=1.3384(9)\,\text{M}_\odot$ and $m_\text{c}=1.3946(9)\,\text{M}_\odot$) plus three tests of general relativity (GR), which the theory passes. The larger mass of the NS companion provides important clues regarding the binary formation of PSR J1757$-$1854. With simulations suggesting 3-$\sigma$ measurements of both the contribution of Lense-Thirring precession to the rate of change of the semi-major axis and the relativistic deformation of the orbit within $\sim7-9$ years, PSR J1757$-$1854 stands out as a unique laboratory for new tests of gravitational theories.

Bibliographical metadata

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
DOIs
Publication statusPublished - 9 Jan 2018