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Title:
Does the accreting millisecond pulsar XTE J1814-338 precess?
Authors:
Chung, C. T. Y.; Galloway, D. K.; Melatos, A.
Affiliation:
AA(School of Physics, University of Melbourne, Parkville, VIC 3010, Australia), AB(School of Physics, Monash University, Clayton, VIC 3800, Australia), AC(School of Physics, University of Melbourne, Parkville, VIC 3010, Australia)
Publication:
A DECADE OF ACCRETING MILLISECOND X-RAY PULSARS. AIP Conference Proceedings, Volume 1068, pp. 47-50 (2008). (AIPC Homepage)
Publication Date:
10/2008
Origin:
AIP
PACS Keywords:
Pulsars, Accretion and accretion disks, X-ray binaries
DOI:
10.1063/1.3031204
Bibliographic Code:
2008AIPC.1068...47C

Abstract

Accretion-powered pulsars with slight ellipticites are expected to precess, producing characteristic variations in their pulse properties. We compute light curves for various geometric configurations of a precessing pulsar and predict the periodic modulation of the mean flux, pulse-phase residuals and fractional amplitudes of the pulse profiles. We then search for these signatures in 37 days of X-ray timing data from the accreting millisecond pulsar XTE J1814-338. We analyze a 12.2-d modulation observed previously and show that it is consistent with a freely precessing neutron star only if the inclination angle is <0.1°, an a priori unlikely orientation. If the observed flux variations are due to precession, we infer an upper limit on ɛ of 3.0×10-9 and estimate the tilt angle θ to lie between 5° and 10° despite the inability of our model to match the relative phasing of the observable parameters. This implies a maximum gravitational wave strain of 10-27 from XTE J1814-338 (assuming a distance of 8 kpc). If the observed flux variations are not due to precession, we place an upper limit on the product V cos θ of <=9.9×10-10.
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