Abstract
From a careful study of 35 high-dispersion spectrograms of P Cygni it is concluded that the spectroscopic data do not confirm the conclusion of Magalashvili and Kharadze that P Cygni is a WUMa type system. It is found that many of the absorption lines are double, the hydrogen absorption lines even triple. This is attributed to line formation in different shells. In the outer shell variations with a period of 114 days lead to observed radial-velocity variations between — 180 and — 240 km/sec. A preliminary conclusion about the velocity field in the atmosphere of P Cygni is drawn and the mass loss is estimated.
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References
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© 1969 D. Reidel Publishing Company, Dordrecht, Holland
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De Groot, M. (1969). Mass Loss from P Cygni. In: Hack, M. (eds) Mass Loss from Stars. Astrophysics and Space Science Library, vol 13. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3405-0_3
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DOI: https://doi.org/10.1007/978-94-010-3405-0_3
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