Optical and UV spectroscopy of the black hole binary candidate LMC X-1

Details Optical and UV spectroscopy of the black hole binary candidate LMC X-1 Optical and UV spectroscopy of the black hole binary candidate LMC X-1

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aj.....94..340h&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 94, Aug. 1987, p. 340-344. NSF-NASA-supported research.

Astronomy and Astrophysics

Astronomy

57

Binary Stars, Black Holes (Astronomy), Stellar Spectrophotometry, Ultraviolet Spectra, Visible Spectrum, Emission Spectra, Iue, Line Spectra, Orbital Elements, Stellar Winds

Scientific paper

Both further optical spectroscopy of the binary star identified with LMC X-1, obtained between 1983 and 1985, and a series of IUE UV spectra taken during a 5 day interval in 1984 are presented. The optical data are used to refine the orbital period to 4.2288 days, and improved orbital parameters are derived. The velocity of the optical emission lines is antiphased with the absorption lines and has twice the velocity amplitude. These new results support the estimates of the masses in the system given earlier. The most probable component masses are approximately 20 solar masses for the primary and near 6 solar masses (for the x-ray star), suggesting the the latter may be a black hole. The UV spectra show very weak, low-velocity stellar-wind lines. It is suggested that much of the surrounding medium is highly ionized by the X-ray flux. The 'nonwind' UV spectral lines and the UV continuum temperature are consistent with the optical data, indicating a late O type star of M(bol) = -8.5. There is a weak modulation of absorption-line strengths with orbital phase, suggestive of a lack of axisymmetry in the X-irradiation of the primary star and indicative of a fairly low orbital inclination.

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