Discovery of a Second Millisecond Accreting Pulsar: XTE J1751–305

By C. Markwardt, J. Swank, T. Strohmayer, J. I. Zand, F. Marshall. 2002

151 citations recorded by the source corpus.

We report the discovery by the Rossi X-Ray Timing Explorer Proportional Counter Array of a second transient accreting millisecond pulsar, XTE J1751-305, during regular monitoring observations of the Galactic bulge region. The pulsar has a spin frequency of 435 Hz, making it one of the fastest pulsars. The pulsations contain the signature of orbital Doppler modulation, which implies an orbital period of 42 minutes, the shortest orbital period of any known radio or X-ray millisecond pulsar. The mass function, fX = (1.278 ± 0.003) × 10-6 M☉, yields a minimum mass for the companion of between 0.013 and 0.017 M☉, depending on the mass of the neutron star. No eclipses were detected. A previous X-ray outburst in 1998 June was discovered in archival All-Sky Monitor data. Assuming mass transfer in this binary system is driven by gravitational radiation, we constrain the orbital inclination to be in the range 30°-85° and the companion mass to be 0.013-0.035 M☉. The companion is most likely a heated helium dwarf. We also present results from the Chandra High Resolution Camera-S observations, which provide the best-known position of XTE J1751-305.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/327440b7112a09ff098249148e10b72acdcaf55b

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Citations in the corpus

Six new candidate ultracompact X-ray binaries (2007, background): “…pulsar, M = accretion-powered millisecond pulsar, B = burster, D = eclipser and/or dipper; a Galloway et al. (2002); b Middleditch et al. (1981); c Markwardt et al. (2002); d Markwardt et al. (2003); e Stella et al. (1987); f Homer et al. (1996); g White & Swank (1982); h Dieball et al. (2005); i…”
Gravitational Radiation from an Accreting Millisecond Pulsar with a Magnetically Confined Mountain (2005, background): “4 3658 (Wijnands & van der Klis 1998; Chakrabarty & Morgan 1998; Galloway et al. 2002; Markwardt et al. 2002).”
THE NEUTRON STAR MASS DISTRIBUTION (2010, background): “…that at least some millisecond pulsars have evolved from a first generation of NSs which have accumulated mass and angular momentum from their evolved companion (Alpar et al. 1982; Radhakrishnan & Srinivasan 1982; Wijnands & van der Klis 1998; Markwardt et al. 2002; Galloway et al. 2002, 2005).”
On the Nature of the X-ray Emission of Accreting Millisecond Pulsar SAX J1808.4-3658 (2002, unknown): “4−3658 (with the periodP = 2.5 ms; Wijnands & van der Klis 1998a), XTE J1751−305 (P = 2.3 ms; Markwardt et al. 2002), XTE J0929−314 (P = 5.4 ms; Galloway et al. 2002) and XTE ⋆ E-mail: juri.poutanen@oulu.fi (JP); Marek.Gierlinski@durham.ac.uk (MG) † Corresponding Fellow, NORDITA,…”
Detecting gravitational wave emission from the known accreting neutron stars (2008, background): “The 2004 outburst of this source, which lasted ≈ 10 days, had total fluence (2-200 keV) (2.5 ± 0.5) × 10−3 ergs cm−2 (Markwardt et al. 2002).”
White Dwarf Donors in Ultracompact Binaries: The Stellar Structure of Finite-Entropy Objects (2003, background): “These masses are significantly greater than those measured in the ultracompact MSPs (Galloway et al. 2002; Markwardt et al. 2002; Bildsten 2002).”