He II 4686-A and H-alpha emission lines of Cygnus X-1

Journal Article · Thu Oct 01 04:00:00 EDT 1987 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/165642· OSTI ID:5748909

Ninkov, Z; Walker, G A.H.; Yang, S

The results of a long-term monitoring program of the He II 4686-A and H-alpha emission lines of the massive X-ray binary Cygnus X-1 are presented. The radial velocities of the residual He II 4686-A emission profiles can be fitted to a smooth sinusoid with little scatter with no significant eccentricity. There is no significant variation in the K amplitude estimated at different epochs which implies a stable origin for the emission. There is a phase lag of 134 deg between the absorption and emission velocity curves. The results support the model of Friend and Castor (1982) in which the primary star almost fills its Roche lobe and has an enhanced mass flow toward the secondary. The He II 4686-A emission strength is strongly modulated with the 5.6-day orbital period. 43 references.

• Research Organization: British Columbia Univ., Vancouver
• OSTI ID: 5748909
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 321; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BALMER LINES
BINARY STARS
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ELEMENTS
EMISSION SPECTRA
FLUIDS
GASES
HELIUM
MASS TRANSFER
NONMETALS
RADIAL VELOCITY
RARE GASES
ROCHE EQUIPOTENTIALS
SPECTRA
STARS
VELOCITY