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Observational evidences of stellar wind

Published online by Cambridge University Press:  12 April 2016

S.P. Tarafdar
S.P. Tarafdar*
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Bombay 400 005, India

Abstract

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Observations mainly from the IUE Spectra of HD 152236 (Blla) have been used to provide support to the various aspects of the theory of stellar wind (SW) and its interaction with the interstellar medium (ISM). Lines arising from excited levels connected radiatively to the ground level tend to be more frequent and/or strong compared to those arising from radiatively forbidden levels of similar excitation as expected from radiatively driven wind. The outward velocity from shifts of Si III lines from different excited levels increases steeply with decreasing excitation energy in agreement with theories. Absorption lines (P-Cygni like) of C II, Al II, Si II and Mg II shifted shortward by about 300 km s-1 suggest an expanding shell around the star. As this velocity is smaller than the terminal velocity (880 km s-1) the circumstellar shell may have been formed as a result of interaction of SW with ISM.

Type
Session I - Winds from Early Type Stars: Observations
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 79 - 82
Copyright
Copyright © Reidel 1981

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