E. D. Grundstrom et al. 2007 ApJ 656 431 doi:10.1086/510508
E. D. Grundstrom1, J. L. Blair1, D. R. Gies1,3, W. Huang1,3,4, M. V. McSwain1,3,5,6, D. Raghavan1, R. L. Riddle1,3,7, J. P. Subasavage1, D. W. Wingert1,3, A. M. Levine2 and R. A. Remillard2
Show affiliationsWe report on a 3 yr spectroscopic monitoring program of the Hα emission in the massive X-ray binary LS I +65 010 = 2S 0114+650, which consists of a B supergiant and a slowly rotating X-ray pulsar. We present revised orbital elements that yield a period of P = 11.5983 ± 0.0006 days and confirm that the orbit has a nonzero eccentricity e = 0.18 ± 0.05. The Hα emission profile is formed in the base of the wind of the B supergiant primary, and we show how this spectral feature varies on timescales that are probably related to the rotational period of the B supergiant. We also examine the X-ray fluxes from the Rossi X-ray Timing Explorer All-Sky Monitor instrument, and we show that the X-ray orbital light curve has a maximum at periastron and a minimum at the inferior conjunction of the B supergiant. We also show that the wind emission strength and the high-energy X-ray flux appear to vary in tandem on timescales of approximately 1 yr.
binaries: spectroscopic; pulsars: individual (2S 0114+650); stars: early-type; stars: individual (LS I +65 010); stars: winds, outflows; supergiants
Issue 1 (2007 February 10)
Received 2006 July 7, accepted for publication 2006 October 27
E. D. Grundstrom et al. 2007 ApJ 656 431
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