Volume 436, Number 2, June III 2005
|Page(s)||661 - 669|
|Section||Stellar structure and evolution|
|Published online||30 May 2005|
VLT/UVES spectroscopy of the O supergiant companion to 4U 1907+09(7)
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: firstname.lastname@example.org
Accepted: 2 March 2005
High-resolution optical spectra of the high-mass X-ray binary 4U 1907+09 covering the wavelength range 4680-10 400 Å indicate that the X-ray pulsar's massive companion is an O8/O9 supergiant with a dense stellar wind. The interstellar atomic lines of and of this strongly reddened source ( mag) are used to set a lower limit to its distance: kpc, excluding the possibility that the massive companion is a Be star. We re-evaluate the system parameters; the new spectral classification of 4U 1907+09's O supergiant companion is discussed in the context of its similarity in X-ray and orbital properties to Wray 15-977/GX 301-2. The Hα line shows variability similar to what is observed in other wind-fed systems. A remarkable feature is the strong He ii 4686 Å emission line, which possibly originates in the accretion flow towards the X-ray pulsar.
Key words: stars: binaries: close / stars: early-type / stars: winds, outflows / X-rays: individual: 4U 1907+09 / ISM: lines and bands
© ESO, 2005
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