A spectroscopic search for colliding stellar winds in O-type close binary systems. III - 29 UW Canis Majoris

Details A spectroscopic search for colliding stellar winds in O-type close binary systems. III - 29 UW Canis Majoris A spectroscopic search for colliding stellar winds in O-type close binary systems. III - 29 UW Canis Majoris

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...407..252w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 407, no. 1, p. 252-265.

Astronomy and Astrophysics

Astrophysics

17

Binary Stars, O Stars, Stellar Spectrophotometry, Stellar Winds, Emission Spectra, H Alpha Line, Radial Velocity, Stellar Spectra, Ultraviolet Spectra

Scientific paper

The orbital-phase variations in the optical emission lines and UV P Cygni lines of the massive O-type binary 29 UW Canis Majoris are investigated in a search for evidence of colliding winds. High SNR spectra of the H-alpha and He I 6678-A emission lines are presented, and radial velocity curves for several features associated with the photosphere of the more luminous primary star are given. The H-alpha features consists of a P Cygni component that shares the motion of the primary, and which probably originates at the base of its wind, and a broad, stationary emission component. It is proposed that the broad emission forms in a plane midway between the stars where the winds collide. A simple geometric model is used to show that this placement of the broad component can explain the lack of orbital velocity shifts, the near-constancy of the emission strength throughout the orbit, the large velocities associated with the H-alpha wings, and the constancy of the velocity range observed.

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