Abstract
The original temporal analysis of a 12 night spectral timeseries of WR-134 has been found to be flawed and a re-analysis shows that the line profile variations are indeed periodic. When combined with a 4 night timeseries taken 45 days earlier, a period near 2.27 d is found in periodograms of the He II λ5412 line centroid, rms line width, and line skew variations. When the emission line residuals are ordered as a function of phase, a sinuous feature appears to “snake” about the line center with an amplitude of ± 500 km s-1. This is ≈ 20 larger than the line centroid amplitude; the calculation of which is heavily weighted by static portions of the line profile. In addition to the “snake,” emission residuals appear that move away from line center on unbound trajectories and are thought to result from the interaction of a periodic driver with the unstable flow of the radiation driven wind. The nature of the periodic driver is a topic for discussion.
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Mccandliss, S.R., Bohannan, B., Robert, C., Moffat, A.F.J. (1994). Erratum: The 2.27 Day Period of WR-134 (HD 191765). In: Moffat, A.F.J., Owocki, S.P., Fullerton, A.W., St-Louis, N. (eds) Instability and Variability of Hot-Star Winds. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0315-2_11
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DOI: https://doi.org/10.1007/978-94-011-0315-2_11
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