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Title:
Rossi X-Ray Timing Explorer and BeppoSAX Observations of the Transient X-Ray Pulsar XTE J1859+083
Authors:
Corbet, R. H. D.; in't Zand, J. J. M.; Levine, A. M.; Marshall, F. E.
Affiliation:
AA(University of Maryland, Baltimore County, MD, USA ; CRESST/Mail Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA ; ), AB(SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, Netherlands ; Astronomical Institute, Utrecht University, P.O. Box 80000, 3508 TA Utrecht, Netherlands ; ), AC(Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA ), AD(Mail Code 660.1, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA)
Publication:
The Astrophysical Journal, Volume 695, Issue 1, pp. 30-35 (2009). (ApJ Homepage)
Publication Date:
04/2009
Origin:
IOP
ApJ Keywords:
stars: individual: XTE J1859+083, stars: neutron, X-rays: binaries
DOI:
10.1088/0004-637X/695/1/30
Bibliographic Code:
2009ApJ...695...30C

Abstract

We present observations of the 9.8 s X-ray pulsar XTE J1859+083 made with the All Sky Monitor (ASM) and Proportional Counter Array (PCA) on board the Rossi X-ray Timing Explorer, and the Wide Field Camera (WFC) on board BeppoSAX. The ASM data cover a 12 year time interval and show that an extended outburst occurred between approximately MJD 50,250 and 50,460 (1996 June 16 to 1997 January 12). The ASM data excluding this outburst interval suggest a possible modulation with a period of 60.65 ± 0.08 days. Eighteen sets of PCA observations were obtained over an approximately one month interval in 1999. The flux variability measured with the PCA appears consistent with the possible period found with the ASM. The PCA measurements of the pulse period showed it to decrease nonmonotonically and then to increase significantly. Doppler shifts due to orbital motion rather than accretion torques appear to be better able to explain the pulse period changes. Observations with the WFC during the extended outburst give a position that is consistent with a previously determined PCA error box, but which has a significantly smaller error. The transient nature of XTE J1859+083 and the length of its pulse period are consistent with it being a Be/neutron star binary. The possible 60.65 day orbital period would be of the expected length for a Be star system with a 9.8 s pulse period.
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