Details

Autor(en) / Beteiligte

• Aldoretta, E. J
• St-Louis, N
• Richardson, N. D
• Moffat, A. F. J
• Eversberg, T
• Hill, G. M
• Shenar, T
• Artigau, É
• Gauza, B
• Knapen, J. H
• Kubát, J
• Kubátová, B
• Maltais-Tariant, R
• Muñoz, M
• Pablo, H
• Ramiaramanantsoa, T
• Richard-Laferrière, A
• Sablowski, D. P
• Simón-Díaz, S
• St-Jean, L
• Bolduan, F
• Dias, F. M
• Dubreuil, P
• Fuchs, D
• Garrel, T
• Grutzeck, G
• Hunger, T
• Küsters, D
• Langenbrink, M
• Leadbeater, R
• Li, D
• Lopez, A
• Mauclaire, B
• Moldenhawer, T
• Potter, M
• dos Santos, E. M
• Schanne, L
• Schmidt, J
• Sieske, H
• Strachan, J
• Stinner, E
• Stinner, P
• Stober, B
• Strandbaek, K
• Syder, T
• Verilhac, D
• Waldschläger, U
• Weiss, D
• Wendt, A

Titel

An extensive spectroscopic time series of three Wolf–Rayet stars – I. The lifetime of large-scale structures in the wind of WR 134

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2016-08, Vol.460 (3), p.3407-3417

Ort / Verlag

London: Oxford University Press

Erscheinungsjahr

2016

Link zum Volltext

Quelle

Alma/SFX Local Collection

Beschreibungen/Notizen

• During the summer of 2013, a 4-month spectroscopic campaign took place to observe the variabilities in three Wolf–Rayet stars. The spectroscopic data have been analysed for WR 134 (WN6b), to better understand its behaviour and long-term periodicity, which we interpret as arising from corotating interaction regions (CIRs) in the wind. By analysing the variability of the He ii λ5411 emission line, the previously identified period was refined to P = 2.255 ± 0.008 (s.d.) d. The coherency time of the variability, which we associate with the lifetime of the CIRs in the wind, was deduced to be 40 ± 6 d, or ∼18 cycles, by cross-correlating the variability patterns as a function of time. When comparing the phased observational grey-scale difference images with theoretical grey-scales previously calculated from models including CIRs in an optically thin stellar wind, we find that two CIRs were likely present. A separation in longitude of Δϕ ≃ 90° was determined between the two CIRs and we suggest that the different maximum velocities that they reach indicate that they emerge from different latitudes. We have also been able to detect observational signatures of the CIRs in other spectral lines (C iv λλ5802,5812 and He i λ5876). Furthermore, a DAC was found to be present simultaneously with the CIR signatures detected in the He i λ5876 emission line which is consistent with the proposed geometry of the large-scale structures in the wind. Small-scale structures also show a presence in the wind, simultaneously with the larger scale structures, showing that they do in fact co-exist.