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An Emission Line Model for AM Herculis Systems: Application to E1405-451

Published online by Cambridge University Press:  25 April 2016

Lilia Ferrario ,
D. T. Wickramasinghe  and
I. R. Tuohy
Lilia Ferrario
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
D. T. Wickramasinghe
Affiliation:
Department of Mathematics, The Australian National University
I. R. Tuohy
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
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Abstract

The optical spectra of the AM Herculis binaries are characterized by extremely complex emission lines whose profiles can be resolved into at least three components which are formed in different regions of the accretion stream leading from the companion star towards the magnetic white dwarf. We present a theoretical model which localizes the formation region of the broad emission line component and provides information regarding the structure of this emitting region. In our model the particle trajectories are integrated in a Roche potential and the volume between the white dwarf and the companion has been divided into two different regimes of motion. In one region the gas escapes from the secondary near the inner Lagrange point and is accelerated along a straight line towards the white dwarf. In the other region the magnetic field is strong enought to divert the gas out of the orbital plane and to channel it towards the white dwarfs surface. The model has been used to interpret radial velocity and velocity dispersion data from the AM Herculis system E1405-451.

Type
Theoretical
Information
Publications of the Astronomical Society of Australia , Volume 7 , Issue 2 , 1987 , pp. 119 - 122
Copyright
Copyright © Astronomical Society of Australia 1987

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