2002/06/30 by D. K. Galloway, Duncan Galloway, Deepto Chakrabarty +4 · 5 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #High-pressure geophysics and materials #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1086/343841
published as Astrophys.J. 576 (2002) L137-L140 · 5 pages, 3 figures; accepted by ApJ Letters. Revised distance lower limit and added a figure showing pulse profiles
arxiv created 2002/08/01 · openalex publication_date 2002/09/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We have identified the third known accretion-powered millisecond pulsar, XTE J0929-314, with the Rossi X-Ray Timing Explorer . The source is a faint, high Galactic latitude X-ray transient ( d ≳ 5 kpc) that was in outburst during 2002 April-June. The 185 Hz (5.4 ms) pulsation had a fractional rms amplitude of 3%-7% and was generally broad and sinusoidal, although occasionally double-peaked. The hard X-ray pulses arrived up to 770 μs earlier than the soft X-ray pulses. The pulsar was spinning down at an average rate of = (-9.2 ± 0.4) × 10 -14 Hz s -1 ; the spin-down torque may arise from magnetic coupling to the accretion disk, a magnetohydrodynamic wind, or gravitational radiation from the rapidly spinning pulsar. The pulsations were modulated by a 43.6 minute ultracompact binary orbit, yielding the smallest measured mass function (2.7 × 10 -7 M ☉ ) of any stellar binary. The binary parameters imply an ≃0.01 M ☉ white dwarf donor and a moderately high inclination. We note that all three known accreting millisecond pulsars are X-ray transients in very close binaries with extremely low mass transfer rates. This is an important clue to the physics governing whether or not persistent millisecond pulsations are detected in low-mass X-ray binaries.