Gravitational Radiation and Rotation of Accreting Neutron Stars
- 1 July 1998
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 501 (1), L89-L93
- https://doi.org/10.1086/311440
Abstract
Recent discoveries by the Rossi X-Ray Timing Explorer indicate that most of the rapidly accreting ( 10−11 M yr−1) weakly magnetic (B1011 G) neutron stars in the Galaxy are rotating at spin frequencies νs 250 Hz. Remarkably, they all rotate in a narrow range of frequencies (no more than a factor of 2, with many within 20% of 300 Hz). I suggest that these stars rotate fast enough so that, on average, the angular momentum added by accretion is lost to gravitational radiation. The strong νs-dependence of the angular momentum loss rate from gravitational radiation then provides a natural reason for similar spin frequencies. Provided that the interior temperature has a large-scale asymmetry misaligned from the spin axis, then the temperature-sensitive electron captures in the deep crust can provide the quadrupole needed ( ~10−7MR2) to reach this limiting situation at νs ≈ 300 Hz. This quadrupole is only present during accretion and makes it difficult to form radio pulsars with νs > (600-800) Hz by accreting at 10−10 M yr−1. The gravity wave strength is hc ~(0.5-1) × 10−26 from many of these neutron stars and greater than 2 × 10−26 for Sco X-1. Prior knowledge of the position, spin frequency, and orbital periods will allow for deep searches for these periodic signals with gravitational wave interferometers (LIGO, VIRGO, and the "dual-recycled" GEO 600 detector), and experimenters need to take such sources into account. Sco X-1 will most likely be detected first.Keywords
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