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Modelling of UV resonance lines

Published online by Cambridge University Press:  14 August 2015

Henny J.G.L.M. Lamers  and
John C. Castor
Henny J.G.L.M. Lamers
Affiliation:
The Astronomical Institute at Utrecht Space Research Laboratory
John C. Castor
Affiliation:
Joint Institute for Laboratory Astrophysics National Bureau of Standards and University of Colorado

Abstract

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The envelopes of early type stars can be studied by comparing observed and theoretical P Cygni profiles of UV resonance lines. The lines are formed by scattering in the expanding envelope and complete frequency redistribution is a reasonable assumption. The Sobolev approximation can be used for the prediction of the profiles, except within a Doppler shift of 2xvthermal from the line center. The profiles are sensitive to the optical depth τrad(v) ∝L ni(r) (dr/dv), but insensitive to the velocity law. We present a fairly simple method to calculate the effects of a photospheric profile or partly overlapping doublets.

Type
Session 2: U.V. Spectroscopy
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 81 - 92
Copyright
Copyright © Reidel 1979 

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