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Ultraviolet Observations of Interacting Binary Be Stars

Published online by Cambridge University Press:  14 August 2015

Geraldine J. Peters  and
Ronald S. Polidan
Geraldine J. Peters
Affiliation:
Department of Astronomy, Univ. of Southern California, Los Angeles, CA 90007 USA
Ronald S. Polidan
Affiliation:
Princeton University Observatory, Princeton, NJ 08540 USA

Abstract

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Initial results from the analysis of a series of timed, high resolution IUE observations of HR 2142, ϕ Per, CX Dra, KX And, AU Mon, and TT Hya are presented. The data base for HR 2142 also includes Copernicus U1 and U2 observations. Variable absorption lines, indicative of mass flow in the system, are observed in all objects except ϕ Per. We also, in general, find evidence of mass outflow in the form of winds and/or discrete components. We observe variable N V absorption in CX Dra and AU Mon and emission features in KX And and ϕ Per (C IV only). U1 data reveals the presence of complex structure in the gas stream in HR 2142. These observations are compared with those of Be stars which are not thought to be interacting binaries.

Type
VII. UV Observations and Mass Loss
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 405 - 409
Copyright
Copyright © Reidel 1982 

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