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Torque Reversal and Spin-Down of the Accretion-Powered Pulsar 4U 1626-67

Chakrabarty, Deepto and Bildsten, Lars and Grunsfeld, John M. and Koh, Danny T. and Prince, Thomas A. and Vaughan, Brian A. and Finger, Mark H. and Scott, D. Matthew and Wilson, Robert B. (1997) Torque Reversal and Spin-Down of the Accretion-Powered Pulsar 4U 1626-67. Astrophysical Journal, 474 (1). Art. No. 414. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20140703-223747001

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Abstract

Over 5 yr of hard X-ray (20-60 keV) monitoring of the 7.66 s accretion-powered pulsar 4U 1626-67 with the Compton Gamma Ray Observatory/BATSE large-area detectors has revealed that the neutron star is now steadily spinning down, in marked contrast to the steady spin-up observed during 1977-1989. This is the second accreting pulsar (the other is GX 1+4) that has shown extended, steady intervals of both spin-up and spin-down. Remarkably, the magnitudes of the spin-up and spin-down torques differ by only 15%, with the neutron star spin changing on a timescale |ν/dot ν| ≈ 5000 yr in both states. The current spin-down rate is itself decreasing on a timescale |dot ν/bar ν| ≈ 26 yr. The long-term timing history shows small-amplitude variations on a 4000 day timescale, which are probably due to variations in the mass transfer rate. The pulsed 20-60 keV emission from 4U 1626-67 is well-fitted by a power-law spectrum with photon index γ = 4.9 and a typical pulsed intensity of 1.5 × 10^(-10) ergs cm^(-2) s^(-1). The low count rates with BATSE prohibited us from constraining the reported 42 minute binary orbit, but we can rule out long-period orbits in the range 2 days lesssim Porb lesssim 900 days. We compare the long-term torque behavior of 4U 1626-67 to other disk-fed accreting pulsars and discuss the implications of our results for the various theories of magnetic accretion torques. The abrupt change in the sign of the torque is difficult to reconcile with the extremely smooth spin-down now observed. The strength of the torque noise in 4U 1626-67, ~10^(-22) Hz^2 s^(-2) Hz^(-1), is the smallest ever measured for an accreting X-ray pulsar, and it is comparable to the timing noise seen in young radio pulsars. We close by pointing out that the core temperature and external torque (the two parameters potentially relevant to internal sources of timing noise) of an accreting neutron star are also comparable to those of young radio pulsars.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/303445DOIArticle
http://iopscience.iop.org/0004-637X/474/1/414/PublisherArticle
http://adsabs.harvard.edu/abs/1997ApJ...474..414CADSArticle
ORCID:
AuthorORCID
Chakrabarty, Deepto0000-0001-8804-8946
Prince, Thomas A.0000-0002-8850-3627
Additional Information:© 1997 American Astronomical Society. Received 1996 March 25, accepted for publication 1996 July 24. It is a pleasure to thank Rob Nelson for useful discussions. We also thank the referee, Michiel van der Klis, for a careful reading of the manuscript. This work was funded in part by NASA grants NAG 5-1458 and NAGW-4517. D. C. was supported by a NASA GSRP Graduate Fellowship under grant NGT-51184 and by a NASA Compton Postdoctoral Fellowship under grant NAG 5-3109. L. B. was supported by Caltech's Lee A. DuBridge Fellowship, funded by the Weingart Foundation; by a NASA Compton Postdoctoral Fellowship under grant NAG 5-2666; and by the Alfred P. Sloan Foundation.
Funders:
Funding AgencyGrant Number
NASANAG 5-1458
NASANAGW-4517
NASANGT-51184
NASA Compton FellowshipNAG 5-3109
Lee A. DuBridge FellowshipUNSPECIFIED
Weingart FoundationUNSPECIFIED
NASA Compton FellowshipNAG 5-2666
Alfred P. Sloan FoundationUNSPECIFIED
Subject Keywords:accretion, accretion disks—binaries: close—pulsars: individual (4U 1626–67)—stars: neutron—X-rays: stars
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1997-01
Issue or Number:1
Record Number:CaltechAUTHORS:20140703-223747001
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140703-223747001
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46851
Collection:CaltechAUTHORS
Deposited By: Deborah Miles
Deposited On:14 Jul 2014 23:13
Last Modified:09 Mar 2020 13:18

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