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Line Profile Modeling of Disks

Published online by Cambridge University Press:  12 April 2016

W. Hummel
W. Hummel*
Affiliation:
Institut für Astronomie und Astrophysik und Universitätssternwarte München, Scheinerstr 1, D–81673 München, Germany

Abstract

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In this talk I give a short overview of models for spectral lines in Be stars disks which I think are quite instructive. I then examine the arguments for my own model assumptions and discuss selected topics concerning radiative line transfer calculations in three dimensions. We show that symmetric Hα emission lines of Be stars can be understood in terms of Keplerian disks. It is also demonstrated that one-armed global disk oscillations provide the best available solution to understand the long-term V/R variations in Be star emission lines.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 396 - 408
Copyright
Copyright © Astronomical Society of the Pacific 2000

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