A 2.3 Day Periodic Variability in the Apparently Single Wolf-Rayet Star WR 134: Collapsed Companion or Rotational Modulation?

• Published in: The Astrophysical journal Vol. 518; no. 1; pp. 428 - 441
• Main Authors: Morel, Thierry, Marchenko, Sergey V, Eenens, Philippe R. J, Moffat, Anthony F. J, Koenigsberger, Gloria, Antokhin, Igor I, Eversberg, Thomas, Tovmassian, Gaghik H, Hill, Grant M, Cardona, Octavio, St-Louis, Nicole
• Format: Journal Article Web Resource
• Language: English
• Published: IOP Publishing 10.06.1999; University of Chicago Press
• Subjects: Aérospatiale, astronomie & astrophysique; Physical, chemical, mathematical & earth Sciences; Physique, chimie, mathématiques & sciences de la terre; Space science, astronomy & astrophysics; STARS: INDIVIDUAL (WR 134); STARS: MASS LOSS; STARS: WOLF-RAYET
• ISSN: 0004-637X; 1538-4357; 1538-4357
• DOI: 10.1086/307250

The apparently single WN 6 type star WR 134 (HD 191765) is distinguished among the Wolf-Rayet star population by its strong, presumably cyclical (P~2.3 day) spectral variations. A true periodicity-which is still very much debated-would render WR 134 a prime candidate for harboring either a collapsed companion or a rotating, large-scale, inhomogeneous outflow. We have carried out an intensive campaign of spectroscopic and photometric monitoring of WR 134 from 1989 to 1997 in an attempt to reveal the true nature of this object. This unprecedentedly large data set allows us to confirm unambiguously the existence of a coherent 2.25+/-0.05 day periodicity in the line-profile changes of He II lambda4686, although the global pattern of variability is different from one epoch to another. This period is only marginally detected in the photometric data set. Assuming the 2.25 day periodic variability to be induced by orbital motion of a collapsed companion, we develop a simple model that aims to investigate (1) the effect of this strongly ionizing, accreting companion on the Wolf-Rayet wind structure, and (2) the expected emergent X-ray luminosity. We argue that the predicted and observed X-ray fluxes can only be matched if the accretion on the collapsed star is significantly inhibited. Additionally, we performed simulations of line-profile variations caused by the orbital revolution of a localized, strongly ionized wind cavity surrounding the X-ray source. A reasonable fit is achieved between the observed and modeled phase-dependent line profiles of He II lambda4686. However, the derived size of the photoionized zone substantially exceeds our expectations, given the observed low-level X-ray flux. Alternatively, we explore rotational modulation of a persistent, largely anisotropic outflow as the origin of the observed cyclical variability. Although qualitative, this hypothesis leads to greater consistency with the observations.