A discussion on VBLUW photometry of the X-ray binary HD 77581 /= VELA X-1 = 3 U 0900-40/ and on the overluminosity of the primaries in X-ray binaries - The optical micro variability of the hot supergiant primaries HD 77581 and HD 153919

Details A discussion on VBLUW photometry of the X-ray binary HD 77581 /= VELA X-1 = 3 U 0900-40/ and on the overluminosity of the primaries in X-ray binaries - The optical micro variability of the hot supergiant primaries HD 77581 and HD 153919 A discussion on VBLUW photometry of the X-ray binary HD 77581 /= VELA X-1 = 3 U 0900-40/ and on the overluminosity of the primaries in X-ray binaries - The optical micro variability of the hot supergiant primaries HD 77581 and HD 153919

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....96...82v&link_type=abstract

Astronomy and Astrophysics, vol. 96, no. 1-2, Mar. 1981, p. 82-90.

Astronomy and Astrophysics

Astrophysics

12

Eclipsing Binary Stars, Light Curve, Stellar Luminosity, Stellar Spectrophotometry, Supergiant Stars, Variable Stars, X Ray Binaries, X Ray Sources, Balmer Series, Hot Stars, Interstellar Extinction, Radial Velocity, Visual Photometry

Scientific paper

A discussion is presented of VBLUW photometry of the X-ray binary HD 77581 (= Vela X-1 = 3 U 0900-40) made in 1976 and 1977. To match all available photometry a period of 8d.9615±0d.0025 seemed to be the best. The light-curve is peculiar with one high peaked maximum, which is variable in height and perhaps also in phase with a time scale of about two years. During this phase of the orbital revolution the star is near periastron, so that more mass flow could occur causing an extra optical flux of at most 0.05 mag. This corresponds to ∼10 times the X-ray luminosity. The size and time scale of the intrinsic scatter around the mean light- and colour curves have been discussed and compared with those of an other X-ray binary HD 153919. Its origin should probably be sought on or near the primary. A comparison of the extremas of light- and radial velocity curve shows inconsistencies, probably caused by several complicating effects. The interstellar reddening as determined by Hammerschlag-Hensberge et al., 1976, E(B-V)J = 0.73 is likely a reliable value. The size of the Balmer jump D is determined and together with Mihalas' (1972) tables of continuum properties it follows that Teff =24,300±200 K and log g = 2.90±0.5. The same has been done for the comparison star HD 76341, which is also a Ib supergiant. The problem of the so-called overluminosity of practically all the primaries of the X-ray binaries, among which HD 77581, has been broached.

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