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Title:
Pushing the Limit on Neutron Star Spin Rates
Authors:
Galloway, D.
Publication:
The Seventh Pacific Rim Conference on Stellar Astrophysics, ASP Conference Series, Vol. 362, Proceedings of the conference held 1-5 November, 2005 in Sejong University, Seoul, Korea. Edited by Y.W. Kang, H.-W. Lee, K.-C. Leung, and K.-S. Cheng. San Francisco: Astronomical Society of the Pacific, 2007., p.105
Publication Date:
06/2007
Origin:
ASP
Bibliographic Code:
2007ASPC..362..105G

Abstract

Millisecond X-ray pulsars consist of a rapidly-spinning neutron star accreting from a low-mass stellar companion and are the long-sought evolutionary progenitors of millisecond radio pulsars, as well as promising candidate sources for gravitational radiation. The population of these sources has grown significantly over the last three years, with the discovery of six new examples to bring the total sample size to seven. Three sources are ultracompact binaries with H-depleted donors and orbital periods of ≈40 min, like the 185 Hz pulsar XTE J0929-314. Three more have orbital periods of 2 hr or longer, similar to IGR J00291+5934, first detected in outburst by INTEGRAL in December 2004. The neutron star in this 2.46 hr binary has the most rapid spin of the accreting pulsars at 599 Hz. The most recently-discovered pulsar, HETE J1900.1-2455 (377 Hz), has an intermediate orbital period of 83.3 min, and has been active for more than 1 yr, much longer than the typical transient outburst. Pulsations were detected only in the first few months of the outburst. This source has since resembled a faint, persistent non-pulsing low-mass X-ray binary, typical of the broader low-mass X-ray binary population.
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