Abstract
Brown et al. (1997) and Ignace et al. (1997) have developed an inversion method to derive the wind velocity distribution from optically thin line profiles formed in spherically symmetric outflows. The method has been applied to three He ii lines (9-7 at 2.83µm, 7-6 at 3.09 µm, and 8-7 at 4.76 µm) observed with the ISO SWS for the stars WR 134 (WN6) and WR 136 (WN6). Of these, the 2.83 µm line probes deepest into the wind owing to the dominant free-free opacity. The winds of both WR 134 and WR 136 have attained only 75% of their respective terminal speeds at the radii where the 2.83 µm line is formed.
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References
Brown, J.C., Richardson, L.L., Cassinelli, J.P., Ignace, R. (1997): A and A 325, 677
Ignace, R., Brown, J.C., Richardson, L.L., Cassinelli, J.P. (1998): A and A 330, 253
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© 1998 Springer-Verlag Berlin Heidelberg
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Ignace, R., Cassinelli, J.P., Morris, P., Brown, J.C. (1998). Using ISO to Probe the Acceleration of Wolf-Rayet Winds. In: Kaper, L., Fullerton, A.W. (eds) Cyclical Variability in Stellar Winds. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-68597-5_4
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DOI: https://doi.org/10.1007/978-3-540-68597-5_4
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