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Observations of velocity fields in WN and Of stars

Published online by Cambridge University Press:  14 August 2015

Virpi S. Niemelä
Virpi S. Niemelä*
Affiliation:
51 y 11, Villa Elisa, Buenos Aires, Argentina

Extract

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Systematic wavelength shifts of series of spectral line centers observed in many early type stars, generally interpreted as due to large scale motions, can give us information about the velocity gradients in stellar atmospheres. However, it should be borne in mind that the velocity gradients inferred from the observed displacements of spectral lines may not correspond to a unique alternative (e.g. see Karp 1978). Also, and especially when we are dealing with stars which have emission lines in their spectra, the structure of the velocity field depends on the assumed temperature structure of the atmosphere, i.e. in which atmospheric region do the lines originate.

Type
Session 8: Evolutionary Scenario and the WR Connection
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 475 - 478
Copyright
Copyright © Reidel 1979 

References

Auer, L.H. and Van Blerkom, D. 1972, Ap. J., 178, 175.CrossRefGoogle Scholar
Conti, P.S. 1977, in IAU Symp. No. 80, in press.CrossRefGoogle Scholar
Conti, P.S., Niemelä, V.S. and Walborn, N.R. 1978, Ap. J., in press.Google Scholar
Karp, A.H. 1978, Ap. J., 222, 578.CrossRefGoogle Scholar
Niemelä, V.S. 1975, in Physics of Movements in Stellar Atmospheres, Coll. No. 250 of C.N.R.S. of France, eds. Cayrel, R. and Steinberg, M., p. 467 Google Scholar
Walborn, N.R. 1973, A.J., 78, 1067.CrossRefGoogle Scholar
Walborn, N.R. 1974, Ap. J., 189, 269.CrossRefGoogle Scholar